https://vmcoolwiki.ipac.caltech.edu/api.php?action=feedcontributions&user=Mattw&feedformat=atom CoolWiki - User contributions [en] 2024-03-29T01:54:47Z User contributions MediaWiki 1.34.2 https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:IC_2118_Current_Research_Activities&diff=2708 Talk:IC 2118 Current Research Activities 2007-12-11T17:46:15Z <p>Mattw: /* 11/30/07 practicing posting */</p> <hr /> <div>== Meeting from 10/9/2007 at Oil City High School ==<br /> <br /> We are going to get started monitoring our brighter T-Tauri candidates and generating light curves for them in the R and I band.<br /> <br /> I (S. Weiser) have selecetd two targets to monitor:<br /> <br /> SSTiau Name is 050511.5-064346, RA = 5h 5m 11.6s, DEC = -6d 43m 46.9s, Rmag = 15.3<br /> <br /> SSTiau Name is 050517.4-063734, RA = 5h 5m 17.5s, DEC = -6d 37m 34.3s, Rmag = 16.7<br /> <br /> Estimated exposure time - 180sec<br /> <br /> Using http://heavens-above.com and The Sky planetarium software I've estimated we will want to be on the telescope in Perth Australia sometime between 3:00 PM and 5:00 PM EST throughout October and November. Does everyone else agree?<br /> <br /> Using the New Mexico Sky telescope (near El Paso, Texas), we will need to be on the telescope between 6:00 AM and 7:30 AM EST. Does everyone agree?<br /> <br /> == Meeting 10/17/07 At OCHS ==<br /> <br /> <br /> These are the Targets I have chosen to monitor.-Nick_<br /> <br /> SSTiau Name is 050730.1-061015, RA=05:07:30.2 DEC= -06:10:15.9<br /> <br /> SSTiau Name is 050730.6-061059, RA=05:07:30.6 DEC= -06:10:59.7<br /> <br /> Exposure time of 180secs, Viewing time from Oil City 2:00pm-5:00pm Est, will be using the Perth Telescope.<br /> <br /> == Telescope Time Reserved ==<br /> <br /> FROM Tim Spuck<br /> <br /> Sandy, I agree with you about the times for Perth and New Mexico Skies. I've reserved the following time in Perth. We can get time on New Mexico Skies as well from the folks at NOAO. Thanks, Mr. Spuck<br /> <br /> October 22 18:00 UT – 20:00 UT<br /> <br /> October 23 18:00 UT – 20:00 UT<br /> <br /> October 24 18:00 UT – 20:00 UT<br /> <br /> October 25 18:00 UT – 20:00 UT<br /> <br /> October 26 18:00 UT – 20:00 UT<br /> <br /> October 27 18:00 UT – 20:00 UT<br /> <br /> October 28 18:00 UT – 20:00 UT<br /> <br /> October 29 18:00 UT – 20:00 UT<br /> <br /> October 30 18:00 UT – 20:00 UT<br /> <br /> October 31 18:00 UT – 20:00 UT<br /> <br /> November 1 17:30 UT – 19:30 UT<br /> <br /> November 2 17:30 UT – 19:30 UT<br /> <br /> November 3 17:30 UT – 19:30 UT<br /> <br /> November 4 17:30 UT – 19:30 UT<br /> <br /> November 5 17:30 UT – 19:30 UT<br /> <br /> November 6 17:30 UT – 19:30 UT<br /> <br /> November 7 17:30 UT – 19:30 UT<br /> <br /> November 8 17:30 UT – 19:30 UT<br /> <br /> November 9 17:30 UT – 19:30 UT<br /> <br /> November 10 17:30 UT – 19:30 UT<br /> <br /> November 11 17:30 UT – 19:30 UT<br /> <br /> November 12 17:30 UT – 19:30 UT<br /> <br /> November 13 17:30 UT – 19:30 UT<br /> <br /> November 14 17:30 UT – 19:30 UT<br /> <br /> November 15 17:00 UT – 19:00 UT<br /> <br /> November 16 17:00 UT – 19:00 UT<br /> <br /> November 17 17:00 UT – 19:00 UT<br /> <br /> November 18 17:00 UT – 19:00 UT<br /> <br /> November 19 17:00 UT – 19:00 UT<br /> <br /> November 20 17:00 UT – 19:00 UT<br /> <br /> == Failed attempt ==<br /> <br /> -Nick-<br /> First attempt to take an image using Perth Failed Due to Weather. 10/17/07<br /> ------------------------------------<br /> <br /> ''X-Dani-''<br /> <br /> My targets are <br /> : 409 RA- 76.854562 5hr7min25.1sec DEC- -6.238076 -6d14m17.1s R Mag17.3<br /> : 412 RA- 76.869411 5hr7min28.7sec DEC- -6.223835 -6d16m36.9s R Mag16.4<br /> : 414 RA- 76.872387 5hr7min29.4sec DEC- -6.276916 -6d16m36.9s R Mag17.3<br /> <br /> == TUTORIAL QUESTIONS ==<br /> ''X-Dani-''<br /> <br /> 1) is it giong to be interactive or informational?<br /> a) are people going to be able to &quot;plug in&quot; the information and it's going to spit out a light curve?<br /> b) is it just going to be a &quot;follow along paper&quot; telling them how to do it step by step?<br /> <br /> == Perth Observing results 10/22/2007 ==<br /> <br /> From Dani ... we tried observing T-Tauri targets using the telescope. Weather looked good at 3:32 PM EST, but telescope stated &quot;Conditions were not sufficient for Observing&quot;. Nick K also tried earlier, but got the same results.<br /> <br /> == Observing Results 10/23/2007 ==<br /> <br /> FROM DANI.... Tried to image at 13:31 EST and this is what it gave me... <br /> &quot;Process Completed<br /> There was a problem with the JPEG preview. See the console log for details. You can go to the logs area to look at or download the run log for this acquisition. <br /> Current Status<br /> RA Dec Az Alt <br /> 09:26:55 -60°00'03&quot; 146° 27° <br /> <br /> Run Journal/Log Output<br /> The script failed. Reasons may include.......<br /> <br /> 1) Its daytime!!! (Perth is GMT + 8 hours)<br /> 2) The weather conditions are not sufficient for observing<br /> 3) The script was aborted by the user<br /> 4) The slew coordinates drifted below the horizon<br /> 5) The scope, camera or both are not connected<br /> 6) REQUEST ABORTED BY ACP<br /> <br /> You can see the dome through our sky camera at .....<br /> http://www.perthobservatory.wa.gov.au/information/po_sky_camera.html<br /> <br /> TRY - AGAIN ..... TRY AGAIN ..... TRY AGAIN&quot; .... this seems to happen alot. it happened to nick also when he tried to image just a few minutes before I did. is something wrong with the telescope? When I checked whether conditions it was clear and the windspeed was at 6.7, so the conditions should have been fine....... i tried again at 13:37 and it stated the same thing. pattern? okay, so it just toldme at 13:39 that the whether conditions were insuffecient or something along those lines... ''what exactly are the ideal conditions?'' [end of Dani post.]<br /> <br /> == Perth failure ==<br /> <br /> From Nick, today I attempted to image my targets at 13:15 est and again at 15:31est. Both times the imaging failed due to some internal problem with the Perth Telescope. I then tried at 16:20est.<br /> <br /> <br /> <br /> From Matt H, I also attempted to image my targets at 16:00 est. At this time the imaging failed for some reason that has to do with Perth Telescope<br /> <br /> <br /> FROMDANI... I also attempted to image and got the same results as Nick and Mattheath<br /> <br /> == Targets for IC2118 ==<br /> <br /> MATTHEATH... #ID SSTiaum Name RA DEC RA DEC R MAG G,S,?<br /> 269 050557.8-064232 76.490978 -6.708933 5 5 57.8 -6 42 32.2 14.6 ?<br /> 283 050608.4-063917 76.535202 -6.654822 5 6 8.4 -6 39 17.4 15.3 ?<br /> <br /> CENTER -- RA : 5h 6m 3.4s DEC : -6d 41m 00s<br /> <br /> <br /> SANDYWEISER....<br /> 192 050511.5-064346 76.298234 -6.72965 5 5 11.7 -6 37 34.3 16.7 S<br /> 200 050517.4-063734 76.322813 -6.626197 5 5 17.5 -6 23 8.5 16.8 ?<br /> <br /> CENTER -- RA : 5h 5m 14.6s DEC : -6d 40m 45s <br /> <br /> ALEXISMCCOOL...<br /> 401 050711.5-061509 76.798211 -6.252738 5 5 7 11.6 -6 15 9.9 15.1 ?<br /> 408 050723.3-061538 76.847362 -6.260664 5 7 23.4 -6 15 38.4 17.0 ?<br /> <br /> CENTER -- RA : 5h 7m 17.6s DEC : -6d 15m 24s<br /> <br /> <br /> DANIYEAGER...<br /> 409 050725.0-061417 76.854562 -6.238076 5 7 25.1 -6 14 17.1 17.3 S<br /> 412 050728.6-061325 76.869411 -6.22385 5 7 28.7 -6 13 25.8 16.4 S<br /> 414 050729.3-061636 76.872387 -6.276916 5 7 29.4 -6 16 36.9 17.3 S<br /> <br /> CENTER -- RA : 5h 7m 28.7s DEC : -6d 13m 25.8s<br /> <br /> NICKKELLEY...<br /> 415 050730.1-061015 76.8757 -6.171072 5 7 30.2 -6 10 15.9 12.2 S<br /> 416 050730.6-061059 76.87754 -6.183262 5 7 30.6 -6 10 59.7 13.5 S<br /> <br /> CENTER -- RA : 5h 7m 44.6s DEC : -6d 9m 54.0s <br /> <br /> CALEMCCLINTOCK...<br /> 430 050800.4-062047 77.001885 -6.346496 5 8 0.5 -6 20 47.4 17.3 S<br /> 434 050809.5-061412 77.039924 -6.236934 5 8 9.6 -6 14 13 16.8 S<br /> <br /> CENTER -- RA : 5h 8m 5s DEC : -6d 17m 30s<br /> <br /> == Perth ==<br /> <br /> -Nick- Once again today Perth was unable to take images, while trying to firgure out the problem with the telescope we e-mailed Perth. They responded saying that there weather sensor had goon bad and they were having trouble with the new one.<br /> <br /> == Failure ==<br /> <br /> Once again today i attempted to image using perth and it is not working due to clouds and wind. Nick-11/08/08<br /> <br /> == First Images 11/09/07 ==<br /> <br /> Today at 1:38est I was able to get the first set of images from Perth. -Nick-<br /> <br /> <br /> ........DANIELLEYEAGER... 11/15/2007_23:57EST<br /> <br /> What images exactly, did you collect? Only your targets or others as well?<br /> <br /> NicK- I collect everyones field when i view, well as many as I have time to get and as long has Perth is corporateing.<br /> <br /> == practice light curve data ==<br /> <br /> ''....DANIELLEYEAGER.. 11/15/2007_23:55EST<br /> <br /> <br /> Would you like our practice light curves posted on here? If so, do you want our entire spread sheets as well as the graph; or just one or the other?........''<br /> <br /> RESPONSE: Dani, yes if you can post them here that would be great. Thanks, Mr. Spuck<br /> <br /> == practice light curve .... ==<br /> <br /> '''''........DANIELLEYEAGER.... 11/19/07 15:11EST'''''<br /> <br /> today during 7th period mr.spuck pulled the IC2118 group aside and discussed how far we had gotten with the practice light curve and the wiki.<br /> <br /> i am almost done with my light curve. i used the HOU [hands on universe] program to collect my data. fast and easy. However, there were only 4 constants in the images, two of which being my targets. once I create the spread sheets along with the graph, I will try to find a way to get them on here along with a step by step on how I did it. <br /> <br /> <br /> '''''15:22EST'''''<br /> <br /> mr.spuck saved a file into the practice folder showing 13 reference points, he also posted them on the wiki in section 17 of the discussion. i'm going to have to go back into my data and force HOU to spit out that information.<br /> <br /> <br /> '''''[END]'''''<br /> <br /> == participants ==<br /> <br /> '''''..................DANIELLEYEAGER'''''<br /> <br /> <br /> <br /> ''mattheath'' <br /> <br /> ''mattwalentosky'' <br /> <br /> ''sandywieser'' <br /> <br /> ''alexismcCool'' <br /> <br /> ''daniyeager'' <br /> <br /> ''calemcClintock''<br /> <br /> ''nickkelley''<br /> <br /> <br /> where is everyone? nick and I seem to be the only ones posting.<br /> <br /> Nick- I agree with Dani if other participants want to be a part of this communication is vital.<br /> <br /> == Location of image files for practice light curve .... ==<br /> <br /> '''''........Spuck.... 11/19/07 15:30EST'''''<br /> All image files are locatde here: http://web.ipac.caltech.edu/staff/rebull/ic2118/monitoring/<br /> <br /> <br /> == X,Y postion of YSO targets and REF objects in images .... ==<br /> <br /> '''''........Spuck.... 11/19/07 15:30EST'''''<br /> <br /> <br /> Using MaxIm DL or Hands On Universe Image Processing Software <br /> <br /> These are the image coordinates for the two YSO targets and 13 common reference objects in the practice light curve data set. <br /> <br /> X Y<br /> <br /> YSO 1: 176, 182 +/- 3 pixels <br /> <br /> YSO 2: 179, 144 +/- 3 pixels <br /> <br /> REF 1: 52, 436 +/- 3 pixels <br /> <br /> REF 2: 94, 124 +/- 3 pixels <br /> <br /> REF 3: 99, 222 +/- 3 pixels <br /> <br /> REF 4: 129, 399 +/- 3 pixels <br /> <br /> REF 5: 131, 309 +/- 3 pixels <br /> <br /> REF 6: 156, 23 +/- 3 pixels <br /> <br /> REF 7: 164, 286 +/- 3 pixels <br /> <br /> REF 8: 201, 35 +/- 3 pixels <br /> <br /> REF 9: 213, 295 +/- 3 pixels <br /> <br /> REF 10: 220, 304 +/- 3 pixels<br /> <br /> REF 11: 290, 36 +/- 3 pixels<br /> <br /> REF 12: 379, 449 +/- 3 pixels<br /> <br /> REF 13: 428, 359 +/- 3 pixels<br /> <br /> == 11/19/2007 ==<br /> <br /> Was able to image targets using Perth- Nick<br /> <br /> == 11/20/2007 ==<br /> <br /> I was able to image both of my targets again today using Perth- Nick<br /> <br /> == 11/21/2007 ==<br /> <br /> Today perth was unable to image my targets due to wind, and then later due to the fact the telescope was already in use. Nick<br /> <br /> == 11/21/2007 ==<br /> <br /> When I image for all the people in the project I get everyones images-Nick<br /> <br /> --[[User:Spuck|Spuck]] 10:53, 4 December 2007 (PST) Nick, rather than saying &quot;everyone&quot;, could you just list the fields and the filters used for each observing session. For Example, list it as: <br /> <br /> Nick's field - R 180 sec, I 180 sec<br /> <br /> Dani's field - R 180 sec, I 180 sec<br /> <br /> Matt's field - R 180 sec, ... got cloudy and I did not get I<br /> <br /> <br /> This way we know exactly what has been imaged.<br /> <br /> == 11-27-17_1333EST ==<br /> <br /> .............DANIELLEYEAGER.....<br /> <br /> <br /> <br /> FIRST ATTEMPT AT POSTING PRACTICE LIGHT CURVE.<br /> <br /> <br /> <br /> note... to load in picture, must upload file to wiki then recall.<br /> <br /> <br /> data table<br /> <br /> <br /> <br /> DATE------------------A------B-------C-------D----RATIO--RATIO C--RATIO D<br /> <br /> 03-13-0803-002...818..1510..5207..8083...1164......4.47.......6.94<br /> <br /> 03-13-0803-001...869..1429..5144..8316...1149......4.48.......7.76<br /> <br /> 03-09-0848-001...760..2853..8800..17440..1806.5....4.73.......9.65<br /> <br /> 03-09-0844-001...727..1024..3927..7418...884.5.....4.44.......8.39<br /> <br /> 03-09-0806-001...976..911...4144..7703...943.5.....4.39.......8.16<br /> <br /> 03-16-0803-001..1271..1179..5153..7797...1225......4.21.......6.36<br /> <br /> 03-15-0810-002..1046..1340..3302..8867...1193......2.77.......7.43<br /> <br /> 03-14-0800-003..1721..2731..10831..19584..2226......4.87......8.8<br /> <br /> 03-14-0800-002..1028..700...5026...8916...864.......5.82.....10.32<br /> <br /> 03-14-0800-001..1158..658...4760...8565...908.......5.24......9.43<br /> <br /> 03-13-0803-003...942..1634..5424...7877...1288......4.21......6.12<br /> <br /> <br /> revised data table<br /> <br /> DATE----------------RATIO C-----RATIO D<br /> <br /> 03-13-0803-002----- 4.47----- 6.94<br /> <br /> 03-13-0803-001----- 4.48----- 7.76<br /> <br /> 03-09-0848-001----- 4.73----- 9.65<br /> <br /> 03-09-0844-001----- 4.44----- 8.39<br /> <br /> 03-09-0806-001----- 4.39----- 8.16<br /> <br /> 03-16-0803-001----- 4.21----- 6.36<br /> <br /> 03-15-0810-002----- 2.77----- 7.43<br /> <br /> 03-14-0800-003----- 4.87----- 8.8<br /> <br /> 03-14-0800-002----- 5.82----- 10.32<br /> <br /> 03-14-0800-001----- 5.24----- 9.43<br /> <br /> 03-13-0803-003----- 4.21----- 6.12<br /> <br /> <br /> [[Image:GRAPH.jpg]]<br /> <br /> <br /> GRAPH IS IMAGE LOADED INTO PHOTOBUCKET.COM AND THEN SAVED TO THE WIKI AS GRAPH.JPG.... THIS IS THE ONLY SOLUTION I COULD COME UP WITH AS TO POSTING A PICTURE OF THE GRAPH. ANY IDEAS OR OTHER OPTIONS??<br /> <br /> .......11/30/07 1017est......... okay, so I made a really REALLY beginner mistake and completly forgot about the fact that I had to use julian date. SOOO.. I will post a new thread with the updated information.<br /> <br /> .....11/30/07 1042EST.............. i guess it's just a day for mistakes. i was using the file image name rather than the date and time from the header. so, i have to do the dates over again AND THEN convert into julian time. <br /> [END OF DANIELLEYEAGER POST]<br /> <br /> <br /> <br /> --[[User:Spuck|Spuck]] 10:45, 4 December 2007 (PST) Dani, when you write ratio C and ratio D, what do you mean? You are dividing what by what? Also, did you follow the directions from the activity we are working showing you how to generate a light curve. In the activity one of the things you are asked to do is convert to Julian time.<br /> <br /> <br /> --[[User:Danielle|Dani]] 10:49, 4 December 2007 (PST) TSpuck, Ratio C means the Candidate C divided by the average of the references. Ratio D means the Candidate D divided by the average of the references. And no, I did not use the activity worksheet. [end]<br /> <br /> == Perth11/27/07 ==<br /> <br /> Once again the Telescope at perth is not imageing.<br /> nick<br /> <br /> == 11/28/07 ==<br /> <br /> Perth is down again today. Unable to acquire new images. 1308est as well as at 1630est Nick.<br /> <br /> == 11/29/07 ==<br /> <br /> Perth is down again today. Unable to acquire new images. 1318est Nick.<br /> <br /> == Practice Light Curve and Loop Problem ==<br /> <br /> ..............DANIELLEYEAGER 11/30/07 1336EST<br /> <br /> After figuring the Julian Date for the data, the light curve started to loop. By loop, I mean that the dates stacked fairly close to right above one another and circled through them forming a loop. By this loop problem, I've made the assumption that if a set of data has several points that are seconds or minutes apart, the data will loop. To solve the loop problem I averaged together the points that formed the loop and had that as my point. Doing so decreased my data points severely, but did work in achieving my desired goal.<br /> <br /> <br /> NOTE .... when uploading pictures make sure to use EXACT title. example.. if the file name is uploaded as graph2.JPG you must type exactly, example capatalizing the JPG.<br /> <br /> NEW DATA TABLE AND GRAPH<br /> <br /> JULIAN DATE..... RATIO C..... RATIO D<br /> <br /> 2454168.838........ 4.52............ 8.73<br /> <br /> 2454172.835........ 4.386...........6.94<br /> <br /> 2454173.833........ 5.31............ 9.52<br /> <br /> 2454174.84.......... 2.77............ 7.43<br /> <br /> 2454175.835........ 4.21............ 6.36<br /> <br /> [[Image:graph2.JPG]]<br /> <br /> <br /> --[[User:Spuck|Spuck]] 11:03, 4 December 2007 (PST) Dani, Can you double check the last two data points on your graph (2454174.84 and 2454175.835)? The curves seem to match up except for one of these two sets. <br /> <br /> Also, does anyone know how to set up a graph in excel so that you only connect some of the data points being graphed? Thanks.<br /> <br /> [END OF DANIELLYEAGER POST]<br /> <br /> == 11/30/07 practicing posting ==<br /> <br /> .......DANIELLYEAGER..... ALEXISMCCOOL... JENNIFERBUTCHART.... 1509 EST<br /> <br /> <br /> to use an image upload file and then insert using the word Image with a colon after words and then the file name, entire thing surrounded by two closed brackets.<br /> <br /> example. <br /> <br /> [[Image:graph2.JPG]]&lt;br&gt;<br /> [nicks image.] [[Image:Graph3.JPG]]<br /> <br /> bullet points<br /> *one<br /> **two<br /> ***three<br /> <br /> You should be commenting on your progress daily to every other day.<br /> <br /> IF YOU HAVE A QUESTION FOR SOMEONE, USE THE FOLLOWING OR A SIMILAR FORMAT.... PERSON'S NAME---type your question.<br /> <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> <br /> Matt's Light Curve using Beth Thomas's Method<br /> <br /> [[Image:Matt.JPG]]<br /> HJD YSO 1 in R YSO 1 in I<br /> <br /> 2454168.838______7703________17560<br /> <br /> 2454172.833______7418________17440<br /> <br /> 2454174.844______8038________19293<br /> <br /> 2454175.835______7869________19316<br /> <br /> 2454177 856______8565________18534<br /> <br /> 2454178 8820_____8820________19204 <br /> <br /> 2454179 8820_____8820________18871 <br /> <br /> 2454180 8820_____8258________18534 <br /> <br /> 2454181 8258_____7820________18310 <br /> <br /> 2454182 7820_____7708________18729<br /> <br /> == 11/30/07__2257 est ==<br /> <br /> .......DANIELLEYEAGER..........<br /> <br /> Access available from fathers house. Security problem under control. It was because of the http's'... does anyone have any questions about the wiki or the practice light curve? post what you can. if you need to, get ahold of me this weekend. Just a quick reminder that all 25 hours must be completly by Friday December 7th. <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> ....JENNIFERBUTCHART.... 1500EST<br /> <br /> TODAY I HAVE BEEN ON GALAXY ZOO IDENTIFYING GALAXIES. ALSO, I HAVE STARTED WORKING ON NAMING THE .FITS FILES THAT MR. SPUCK GAVE ME. I AM STILL HAVING A LITTLE TROUBLE WITH THE Sb GALAXIES BUT OTHER THAN THAT, EVERYTHING IS OKAY. <br /> <br /> --[[User:Spuck|Spuck]] 11:07, 4 December 2007 (PST) Jennifer, FYI discussions on the Taurus Galaxy project will now take place in a different part of the Wiki. Go to the discussion page off of the [https://coolwiki.ipac.caltech.edu/index.php/Galaxy_Classification Galaxy Clasification Page]. And know you should not have known that at this point :). Thanks.<br /> <br /> [END JENNIFERBUTCHART POST.]<br /> <br /> == 12/02/07_1554 est ==<br /> <br /> ...DANIELLEYEAGER....<br /> <br /> Jennifer, good job on posting, but from now on, please try to open up a new thread unless what you are posting applys directly to the previous post. Did you have any problems posting?<br /> <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> == 12/02/07_1604 est ==<br /> <br /> ....DANIELLEYEAGER......<br /> <br /> Tried to get on perth and take some images. Telescope was in use by perth. I did go into the images we have already taken and saved some of the images titled Daniscandidates to my personal computer. I don't really know what to do with them though. How many pictures do we have that are focused on my center? Should I start getting the data pulled together and working on my real light curve now that I am finished with my practice light curve? Or should I simply focus on mastering the wiki?<br /> <br /> --[[User:Spuck|Spuck]] 11:18, 4 December 2007 (PST) Dani, you're doing a great job with the Wiki. Unfortunately the Perth Telescope is down for now. I just found out today that the RA motor went bad in the mount. I will post more news as I get it. We will probably have to start using New Mexico Skies telescope for our observations. This means being up at 2:00 AM EST ... any volunteers? For now, why don't you focus on working with the rest of the team ... bringing them up to spped on how to access and use the Wiki, as well as working through the Wiki to see what we should focus on in our AAS Poster.<br /> <br /> 1615 est<br /> <br /> While trying to save over my images, when clicked, some files opened to a page showing the picture directly, where as others had a prompt coming up asking whether I wanted to find the image or save the image. Why?<br /> <br /> --[[User:Spuck|Spuck]] 11:18, 4 December 2007 (PST) Dani, I'm not sure. WHy don't you show me this when you have a chance. Thanks.<br /> <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> == 12/2/07_2226 est ==<br /> <br /> ......DANIELLEYEAGER.....<br /> <br /> dumbie me, i went to log on and do some imaging, but then i realised that it was like.. 10 in the morning. so keep in mind when imaging the +12 to +13 hour time difference.<br /> <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> == Highlights of Wiki for Poster at AAS ==<br /> <br /> ....DANIELLEYEAGER 12/03/07 1036 est....<br /> <br /> Newest part of the project = Find 'interesting' or 'important' parts of the wiki to highlight on poster. You can post parts you would like to use in this thread. ''[If you don't remember how to post on a particular thread, you click edit to the left of the heading of the thread you want to post. If you want to start a new thread, scroll to the top and click on the + (plus) sign beside the tab for edit. And as always, if you have questions on the wiki, type my name in caps and then your question.]''<br /> <br /> <br /> <br /> Example / Rough Draft of poster.<br /> <br /> [[Image:Slide1.JPG]]<br /> <br /> [END OF INTRODUCTION, POST BELOW.]<br /> ___________________________________________________________________________<br /> <br /> <br /> .....DANIELLEYEAGER 12/03/07 1253 EST...<br /> <br /> *Basics on the fact that you are working on real research, and at the same time it is an informational, so if you have questions, nice times out of ten, the information is right there for you to get and work with. [Main page.]<br /> <br /> *A lot of time we work with IR and if someone didn’t know what IR is, we have a section specifically noted for that. [Main Page, section 3]<br /> <br /> *Future research project, Galaxy Classifications. <br /> <br /> *Main page section 8.<br /> <br /> *Users Guide on the bottom of the Main Page.<br /> <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> Nick Kelley 12/03/07 1342 est<br /> <br /> *Past T-Tauri work.<br /> <br /> *Things the wiki allows use to do better.<br /> <br /> *Interaction with other students<br /> <br /> *Allows real Scientific work to be done by students.<br /> <br /> --[[User:Spuck|Spuck]] 11:55, 4 December 2007 (PST) These are great ideas ... keep them coming. Also we have a knew location in the WIKI for posting ideas for the 2008 AAS Wiki poster ideas and work items. SO, please post at the [https://coolwiki.ipac.caltech.edu/index.php/Working_area_for_AAS_jan_2008_poster AAS Wiki Poster Page] in the future. Thanks.<br /> <br /> == Practice curve ==<br /> <br /> Nick's light curve, 12/04/07 1:34<br /> <br /> Julian Date Ratio 1 Ratio 2<br /> 2454172.835 4.4 7<br /> 2454173.833 5.3 9.5<br /> 2454174.843 3.6 7.2<br /> 2454175.835 4.2 6.4<br /> <br /> <br /> <br /> [[Image:Graph3.JPG]]<br /> <br /> Once again Perth is down.<br /> <br /> --[[User:Spuck|Spuck]] 11:39, 4 December 2007 (PST) Nick, Perth will probably be down for a bit. See my previous post to Dani. Also, your light curve looks similar to Dani's. That's good and bad. :) Can you check with Dani and answer the following question for me and then post your responses:<br /> <br /> 1. Did the two of you use all the same reference stars?<br /> <br /> 2. Did the two of you use the same software to get the brightness values for your reference stars and YSO candidates?<br /> <br /> Also, I'd like to se you modify your graph a bit. Label the Y axis more clearly (don't just say ratio ... ratio of what?). Also, turn the julian dates (ie. like I had Dani do hers). And use the scatter plot with the line connecting the data points. Also correct your spelling error in the graph title. Thanks.<br /> <br /> --[[User:Nicholas|Nicholas]] 10:36, 6 December 2007 (PST) Well Mr. Spuck Dani walked me through what to do with the Light Curve so it would be understandable why our light curves would be similar. [end]<br /> <br /> --[[User:Danielle|DanielleYeager]] 09:59, 7 December 2007 (PST) 1.) I don't know if we used the same reference stars, but I do know that he used MORE reference stars than I did.<br /> <br /> 2.) I used HOU.<br /> <br /> ==12/3/07_2048 est==<br /> ....JENNIFERBUTCHART....2048EST<br /> <br /> Today, stayed after with Alexis, Danielle, Cale, and Alix in Mr. Spuck's room. Took notes on basics of things for the Austin trip. Parents signed the permission slip and are pleased with the trip. Mom's meeting with Mr. Spuck went well, obviously.<br /> <br /> 2:40-5:10, worked on galaxy research.<br /> <br /> Tomorrow, doing notes on the book Mr. Spuck gave me. <br /> <br /> I officially have my hours as of today. :)<br /> <br /> --[[User:Spuck|Spuck]] 11:29, 4 December 2007 (PST) Jennifer, I'll need to see the log of your hours sometime before friday. Also, why don't you type up the notes from our discussion and get them posted on to the galaxy classification board. You can make the graphics in paint, or draw and scan them in, or use a digital camera to take pics of your notes and upload the graphics. Either way is fine with me.<br /> <br /> [END JENNIFERBUTCHART POST.]<br /> <br /> <br /> <br /> .. DANIELLEYEAGER 12/04/07 ..<br /> <br /> Jennifer, again, good job on posting, but please post in the Galaxy section, if you need a refresher on how to get to it, from the main page go to Future Research Projects and then from there Galaxy then discussion. I beleive that is the route.<br /> <br /> --[[User:Spuck|Spuck]] 11:25, 4 December 2007 (PST) FYI ... here is the link again to the Go to the discussion page off of the [https://coolwiki.ipac.caltech.edu/index.php/Galaxy_Classification Galaxy Clasification Page]. <br /> <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> == 12/04/07 1349 est ==<br /> <br /> '''''UPDATE IN HOW TO POST PLEASE READ'''''<br /> <br /> <br /> --[[User:Danielle|Dani]] 10:53, 4 December 2007 (PST)When posting, rather than typing your name and time, simply click the icon above the Subject/Headling square that looks like a squiggle. It is the second icon from the right. Click that before you start your post, it will post your name date and time for you. and then at the end of the post, simply type [end]<br /> <br /> --[[User:Spuck|Spuck]] 12:08, 4 December 2007 (PST) This is a very useful tool, so please use it. This is what it looks like on your editing screen:<br /> <br /> [[Image:timestamp.jpg]] [end]<br /> <br /> --[[User:Danielle|DanielleYeager]] 07:34, 5 December 2007 (PST) How do you do a screen shot? .. if you go into your preferences and change your 'nickname' it changes what comes up as your name for your signature.[end]<br /> <br /> --[[User:Nicholas|NicholasJamesKelley]] 10:17, 7 December 2007 (PST) Perth is down at the moment and has been for a couple of days and will continue to be for an indefinite period of time. This is a very depressing bit of info because it not only sets back the spitzer project as a whole but also sets back my and other individual's projects for the Pittsburgh Regional Science and Engineering Fair.<br /> <br /> == Light Curve Correction ==<br /> <br /> --[[User:Danielle|DanielleYeager]] 10:44, 7 December 2007 (PST) In study of both Nick's and my own light curve, we have discovered why the peaks are not matching up. The graphs show two different candidates rather than two different filters for the same candidate. Both light curves need redone, focusing on one candidate in both the I and the R filters. Each graph needs to show the I and R light curve for one candidate. [end]<br /> <br /> --[[User:Nicholas|NicholasJamesKelley]] 10:47, 7 December 2007 (PST) These are my light curves for the 2 candidates that I am monitoring for Spitzer and the Sceince fair. I am currently monitoring to get more accurate curves to take with me.<br /> <br /> <br /> <br /> Candidate <br /> 415 Julian Date I Ratio R Ratio<br /> 12-Feb 2454144.168 1.20 <br /> 21-Feb 2454153.051 1.32 0.6<br /> 22-Feb 2454154.144 1.6 0.63<br /> 23-Feb 2454155.121 1.76 0.84<br /> 27-Feb 2454158.9 1.27 0.53<br /> 6-Mar 2454166.035 1.33 0.56<br /> 9-Mar 2454169.047 1.66 0.73<br /> 11-Mar 2454171.074 1.49 0.68<br /> 12-Mar 2454172.013 1.5 0.65<br /> 16-Mar 2454176.01 0.96 0.45<br /> <br /> [[Image:415.JPG]]<br /> <br /> Candidate <br /> 416 Julian Date I ratio R ratio<br /> 12-Feb 2454144.168 3 <br /> 21-Feb 2454153.051 3.04 1.3<br /> 22-Feb 2454154.144 3.06 1.19<br /> 23-Feb 2454155.121 2.86 1.31<br /> 27-Feb 2454158.9 3.24 1.4<br /> 6-Mar 2454166.035 3.26 1.52<br /> 9-Mar 2454169.047 3.07 1.31<br /> 11-Mar 2454171.074 3.07 1.33<br /> 12-Mar 2454172.013 3.36 1.44<br /> 16-Mar 2454176.01 3.2 1.38<br /> <br /> [[Image:416.JPG]]</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:IC_2118_Current_Research_Activities&diff=2707 Talk:IC 2118 Current Research Activities 2007-12-11T17:29:04Z <p>Mattw: /* 11/30/07 practicing posting */</p> <hr /> <div>== Meeting from 10/9/2007 at Oil City High School ==<br /> <br /> We are going to get started monitoring our brighter T-Tauri candidates and generating light curves for them in the R and I band.<br /> <br /> I (S. Weiser) have selecetd two targets to monitor:<br /> <br /> SSTiau Name is 050511.5-064346, RA = 5h 5m 11.6s, DEC = -6d 43m 46.9s, Rmag = 15.3<br /> <br /> SSTiau Name is 050517.4-063734, RA = 5h 5m 17.5s, DEC = -6d 37m 34.3s, Rmag = 16.7<br /> <br /> Estimated exposure time - 180sec<br /> <br /> Using http://heavens-above.com and The Sky planetarium software I've estimated we will want to be on the telescope in Perth Australia sometime between 3:00 PM and 5:00 PM EST throughout October and November. Does everyone else agree?<br /> <br /> Using the New Mexico Sky telescope (near El Paso, Texas), we will need to be on the telescope between 6:00 AM and 7:30 AM EST. Does everyone agree?<br /> <br /> == Meeting 10/17/07 At OCHS ==<br /> <br /> <br /> These are the Targets I have chosen to monitor.-Nick_<br /> <br /> SSTiau Name is 050730.1-061015, RA=05:07:30.2 DEC= -06:10:15.9<br /> <br /> SSTiau Name is 050730.6-061059, RA=05:07:30.6 DEC= -06:10:59.7<br /> <br /> Exposure time of 180secs, Viewing time from Oil City 2:00pm-5:00pm Est, will be using the Perth Telescope.<br /> <br /> == Telescope Time Reserved ==<br /> <br /> FROM Tim Spuck<br /> <br /> Sandy, I agree with you about the times for Perth and New Mexico Skies. I've reserved the following time in Perth. We can get time on New Mexico Skies as well from the folks at NOAO. Thanks, Mr. Spuck<br /> <br /> October 22 18:00 UT – 20:00 UT<br /> <br /> October 23 18:00 UT – 20:00 UT<br /> <br /> October 24 18:00 UT – 20:00 UT<br /> <br /> October 25 18:00 UT – 20:00 UT<br /> <br /> October 26 18:00 UT – 20:00 UT<br /> <br /> October 27 18:00 UT – 20:00 UT<br /> <br /> October 28 18:00 UT – 20:00 UT<br /> <br /> October 29 18:00 UT – 20:00 UT<br /> <br /> October 30 18:00 UT – 20:00 UT<br /> <br /> October 31 18:00 UT – 20:00 UT<br /> <br /> November 1 17:30 UT – 19:30 UT<br /> <br /> November 2 17:30 UT – 19:30 UT<br /> <br /> November 3 17:30 UT – 19:30 UT<br /> <br /> November 4 17:30 UT – 19:30 UT<br /> <br /> November 5 17:30 UT – 19:30 UT<br /> <br /> November 6 17:30 UT – 19:30 UT<br /> <br /> November 7 17:30 UT – 19:30 UT<br /> <br /> November 8 17:30 UT – 19:30 UT<br /> <br /> November 9 17:30 UT – 19:30 UT<br /> <br /> November 10 17:30 UT – 19:30 UT<br /> <br /> November 11 17:30 UT – 19:30 UT<br /> <br /> November 12 17:30 UT – 19:30 UT<br /> <br /> November 13 17:30 UT – 19:30 UT<br /> <br /> November 14 17:30 UT – 19:30 UT<br /> <br /> November 15 17:00 UT – 19:00 UT<br /> <br /> November 16 17:00 UT – 19:00 UT<br /> <br /> November 17 17:00 UT – 19:00 UT<br /> <br /> November 18 17:00 UT – 19:00 UT<br /> <br /> November 19 17:00 UT – 19:00 UT<br /> <br /> November 20 17:00 UT – 19:00 UT<br /> <br /> == Failed attempt ==<br /> <br /> -Nick-<br /> First attempt to take an image using Perth Failed Due to Weather. 10/17/07<br /> ------------------------------------<br /> <br /> ''X-Dani-''<br /> <br /> My targets are <br /> : 409 RA- 76.854562 5hr7min25.1sec DEC- -6.238076 -6d14m17.1s R Mag17.3<br /> : 412 RA- 76.869411 5hr7min28.7sec DEC- -6.223835 -6d16m36.9s R Mag16.4<br /> : 414 RA- 76.872387 5hr7min29.4sec DEC- -6.276916 -6d16m36.9s R Mag17.3<br /> <br /> == TUTORIAL QUESTIONS ==<br /> ''X-Dani-''<br /> <br /> 1) is it giong to be interactive or informational?<br /> a) are people going to be able to &quot;plug in&quot; the information and it's going to spit out a light curve?<br /> b) is it just going to be a &quot;follow along paper&quot; telling them how to do it step by step?<br /> <br /> == Perth Observing results 10/22/2007 ==<br /> <br /> From Dani ... we tried observing T-Tauri targets using the telescope. Weather looked good at 3:32 PM EST, but telescope stated &quot;Conditions were not sufficient for Observing&quot;. Nick K also tried earlier, but got the same results.<br /> <br /> == Observing Results 10/23/2007 ==<br /> <br /> FROM DANI.... Tried to image at 13:31 EST and this is what it gave me... <br /> &quot;Process Completed<br /> There was a problem with the JPEG preview. See the console log for details. You can go to the logs area to look at or download the run log for this acquisition. <br /> Current Status<br /> RA Dec Az Alt <br /> 09:26:55 -60°00'03&quot; 146° 27° <br /> <br /> Run Journal/Log Output<br /> The script failed. Reasons may include.......<br /> <br /> 1) Its daytime!!! (Perth is GMT + 8 hours)<br /> 2) The weather conditions are not sufficient for observing<br /> 3) The script was aborted by the user<br /> 4) The slew coordinates drifted below the horizon<br /> 5) The scope, camera or both are not connected<br /> 6) REQUEST ABORTED BY ACP<br /> <br /> You can see the dome through our sky camera at .....<br /> http://www.perthobservatory.wa.gov.au/information/po_sky_camera.html<br /> <br /> TRY - AGAIN ..... TRY AGAIN ..... TRY AGAIN&quot; .... this seems to happen alot. it happened to nick also when he tried to image just a few minutes before I did. is something wrong with the telescope? When I checked whether conditions it was clear and the windspeed was at 6.7, so the conditions should have been fine....... i tried again at 13:37 and it stated the same thing. pattern? okay, so it just toldme at 13:39 that the whether conditions were insuffecient or something along those lines... ''what exactly are the ideal conditions?'' [end of Dani post.]<br /> <br /> == Perth failure ==<br /> <br /> From Nick, today I attempted to image my targets at 13:15 est and again at 15:31est. Both times the imaging failed due to some internal problem with the Perth Telescope. I then tried at 16:20est.<br /> <br /> <br /> <br /> From Matt H, I also attempted to image my targets at 16:00 est. At this time the imaging failed for some reason that has to do with Perth Telescope<br /> <br /> <br /> FROMDANI... I also attempted to image and got the same results as Nick and Mattheath<br /> <br /> == Targets for IC2118 ==<br /> <br /> MATTHEATH... #ID SSTiaum Name RA DEC RA DEC R MAG G,S,?<br /> 269 050557.8-064232 76.490978 -6.708933 5 5 57.8 -6 42 32.2 14.6 ?<br /> 283 050608.4-063917 76.535202 -6.654822 5 6 8.4 -6 39 17.4 15.3 ?<br /> <br /> CENTER -- RA : 5h 6m 3.4s DEC : -6d 41m 00s<br /> <br /> <br /> SANDYWEISER....<br /> 192 050511.5-064346 76.298234 -6.72965 5 5 11.7 -6 37 34.3 16.7 S<br /> 200 050517.4-063734 76.322813 -6.626197 5 5 17.5 -6 23 8.5 16.8 ?<br /> <br /> CENTER -- RA : 5h 5m 14.6s DEC : -6d 40m 45s <br /> <br /> ALEXISMCCOOL...<br /> 401 050711.5-061509 76.798211 -6.252738 5 5 7 11.6 -6 15 9.9 15.1 ?<br /> 408 050723.3-061538 76.847362 -6.260664 5 7 23.4 -6 15 38.4 17.0 ?<br /> <br /> CENTER -- RA : 5h 7m 17.6s DEC : -6d 15m 24s<br /> <br /> <br /> DANIYEAGER...<br /> 409 050725.0-061417 76.854562 -6.238076 5 7 25.1 -6 14 17.1 17.3 S<br /> 412 050728.6-061325 76.869411 -6.22385 5 7 28.7 -6 13 25.8 16.4 S<br /> 414 050729.3-061636 76.872387 -6.276916 5 7 29.4 -6 16 36.9 17.3 S<br /> <br /> CENTER -- RA : 5h 7m 28.7s DEC : -6d 13m 25.8s<br /> <br /> NICKKELLEY...<br /> 415 050730.1-061015 76.8757 -6.171072 5 7 30.2 -6 10 15.9 12.2 S<br /> 416 050730.6-061059 76.87754 -6.183262 5 7 30.6 -6 10 59.7 13.5 S<br /> <br /> CENTER -- RA : 5h 7m 44.6s DEC : -6d 9m 54.0s <br /> <br /> CALEMCCLINTOCK...<br /> 430 050800.4-062047 77.001885 -6.346496 5 8 0.5 -6 20 47.4 17.3 S<br /> 434 050809.5-061412 77.039924 -6.236934 5 8 9.6 -6 14 13 16.8 S<br /> <br /> CENTER -- RA : 5h 8m 5s DEC : -6d 17m 30s<br /> <br /> == Perth ==<br /> <br /> -Nick- Once again today Perth was unable to take images, while trying to firgure out the problem with the telescope we e-mailed Perth. They responded saying that there weather sensor had goon bad and they were having trouble with the new one.<br /> <br /> == Failure ==<br /> <br /> Once again today i attempted to image using perth and it is not working due to clouds and wind. Nick-11/08/08<br /> <br /> == First Images 11/09/07 ==<br /> <br /> Today at 1:38est I was able to get the first set of images from Perth. -Nick-<br /> <br /> <br /> ........DANIELLEYEAGER... 11/15/2007_23:57EST<br /> <br /> What images exactly, did you collect? Only your targets or others as well?<br /> <br /> NicK- I collect everyones field when i view, well as many as I have time to get and as long has Perth is corporateing.<br /> <br /> == practice light curve data ==<br /> <br /> ''....DANIELLEYEAGER.. 11/15/2007_23:55EST<br /> <br /> <br /> Would you like our practice light curves posted on here? If so, do you want our entire spread sheets as well as the graph; or just one or the other?........''<br /> <br /> RESPONSE: Dani, yes if you can post them here that would be great. Thanks, Mr. Spuck<br /> <br /> == practice light curve .... ==<br /> <br /> '''''........DANIELLEYEAGER.... 11/19/07 15:11EST'''''<br /> <br /> today during 7th period mr.spuck pulled the IC2118 group aside and discussed how far we had gotten with the practice light curve and the wiki.<br /> <br /> i am almost done with my light curve. i used the HOU [hands on universe] program to collect my data. fast and easy. However, there were only 4 constants in the images, two of which being my targets. once I create the spread sheets along with the graph, I will try to find a way to get them on here along with a step by step on how I did it. <br /> <br /> <br /> '''''15:22EST'''''<br /> <br /> mr.spuck saved a file into the practice folder showing 13 reference points, he also posted them on the wiki in section 17 of the discussion. i'm going to have to go back into my data and force HOU to spit out that information.<br /> <br /> <br /> '''''[END]'''''<br /> <br /> == participants ==<br /> <br /> '''''..................DANIELLEYEAGER'''''<br /> <br /> <br /> <br /> ''mattheath'' <br /> <br /> ''mattwalentosky'' <br /> <br /> ''sandywieser'' <br /> <br /> ''alexismcCool'' <br /> <br /> ''daniyeager'' <br /> <br /> ''calemcClintock''<br /> <br /> ''nickkelley''<br /> <br /> <br /> where is everyone? nick and I seem to be the only ones posting.<br /> <br /> Nick- I agree with Dani if other participants want to be a part of this communication is vital.<br /> <br /> == Location of image files for practice light curve .... ==<br /> <br /> '''''........Spuck.... 11/19/07 15:30EST'''''<br /> All image files are locatde here: http://web.ipac.caltech.edu/staff/rebull/ic2118/monitoring/<br /> <br /> <br /> == X,Y postion of YSO targets and REF objects in images .... ==<br /> <br /> '''''........Spuck.... 11/19/07 15:30EST'''''<br /> <br /> <br /> Using MaxIm DL or Hands On Universe Image Processing Software <br /> <br /> These are the image coordinates for the two YSO targets and 13 common reference objects in the practice light curve data set. <br /> <br /> X Y<br /> <br /> YSO 1: 176, 182 +/- 3 pixels <br /> <br /> YSO 2: 179, 144 +/- 3 pixels <br /> <br /> REF 1: 52, 436 +/- 3 pixels <br /> <br /> REF 2: 94, 124 +/- 3 pixels <br /> <br /> REF 3: 99, 222 +/- 3 pixels <br /> <br /> REF 4: 129, 399 +/- 3 pixels <br /> <br /> REF 5: 131, 309 +/- 3 pixels <br /> <br /> REF 6: 156, 23 +/- 3 pixels <br /> <br /> REF 7: 164, 286 +/- 3 pixels <br /> <br /> REF 8: 201, 35 +/- 3 pixels <br /> <br /> REF 9: 213, 295 +/- 3 pixels <br /> <br /> REF 10: 220, 304 +/- 3 pixels<br /> <br /> REF 11: 290, 36 +/- 3 pixels<br /> <br /> REF 12: 379, 449 +/- 3 pixels<br /> <br /> REF 13: 428, 359 +/- 3 pixels<br /> <br /> == 11/19/2007 ==<br /> <br /> Was able to image targets using Perth- Nick<br /> <br /> == 11/20/2007 ==<br /> <br /> I was able to image both of my targets again today using Perth- Nick<br /> <br /> == 11/21/2007 ==<br /> <br /> Today perth was unable to image my targets due to wind, and then later due to the fact the telescope was already in use. Nick<br /> <br /> == 11/21/2007 ==<br /> <br /> When I image for all the people in the project I get everyones images-Nick<br /> <br /> --[[User:Spuck|Spuck]] 10:53, 4 December 2007 (PST) Nick, rather than saying &quot;everyone&quot;, could you just list the fields and the filters used for each observing session. For Example, list it as: <br /> <br /> Nick's field - R 180 sec, I 180 sec<br /> <br /> Dani's field - R 180 sec, I 180 sec<br /> <br /> Matt's field - R 180 sec, ... got cloudy and I did not get I<br /> <br /> <br /> This way we know exactly what has been imaged.<br /> <br /> == 11-27-17_1333EST ==<br /> <br /> .............DANIELLEYEAGER.....<br /> <br /> <br /> <br /> FIRST ATTEMPT AT POSTING PRACTICE LIGHT CURVE.<br /> <br /> <br /> <br /> note... to load in picture, must upload file to wiki then recall.<br /> <br /> <br /> data table<br /> <br /> <br /> <br /> DATE------------------A------B-------C-------D----RATIO--RATIO C--RATIO D<br /> <br /> 03-13-0803-002...818..1510..5207..8083...1164......4.47.......6.94<br /> <br /> 03-13-0803-001...869..1429..5144..8316...1149......4.48.......7.76<br /> <br /> 03-09-0848-001...760..2853..8800..17440..1806.5....4.73.......9.65<br /> <br /> 03-09-0844-001...727..1024..3927..7418...884.5.....4.44.......8.39<br /> <br /> 03-09-0806-001...976..911...4144..7703...943.5.....4.39.......8.16<br /> <br /> 03-16-0803-001..1271..1179..5153..7797...1225......4.21.......6.36<br /> <br /> 03-15-0810-002..1046..1340..3302..8867...1193......2.77.......7.43<br /> <br /> 03-14-0800-003..1721..2731..10831..19584..2226......4.87......8.8<br /> <br /> 03-14-0800-002..1028..700...5026...8916...864.......5.82.....10.32<br /> <br /> 03-14-0800-001..1158..658...4760...8565...908.......5.24......9.43<br /> <br /> 03-13-0803-003...942..1634..5424...7877...1288......4.21......6.12<br /> <br /> <br /> revised data table<br /> <br /> DATE----------------RATIO C-----RATIO D<br /> <br /> 03-13-0803-002----- 4.47----- 6.94<br /> <br /> 03-13-0803-001----- 4.48----- 7.76<br /> <br /> 03-09-0848-001----- 4.73----- 9.65<br /> <br /> 03-09-0844-001----- 4.44----- 8.39<br /> <br /> 03-09-0806-001----- 4.39----- 8.16<br /> <br /> 03-16-0803-001----- 4.21----- 6.36<br /> <br /> 03-15-0810-002----- 2.77----- 7.43<br /> <br /> 03-14-0800-003----- 4.87----- 8.8<br /> <br /> 03-14-0800-002----- 5.82----- 10.32<br /> <br /> 03-14-0800-001----- 5.24----- 9.43<br /> <br /> 03-13-0803-003----- 4.21----- 6.12<br /> <br /> <br /> [[Image:GRAPH.jpg]]<br /> <br /> <br /> GRAPH IS IMAGE LOADED INTO PHOTOBUCKET.COM AND THEN SAVED TO THE WIKI AS GRAPH.JPG.... THIS IS THE ONLY SOLUTION I COULD COME UP WITH AS TO POSTING A PICTURE OF THE GRAPH. ANY IDEAS OR OTHER OPTIONS??<br /> <br /> .......11/30/07 1017est......... okay, so I made a really REALLY beginner mistake and completly forgot about the fact that I had to use julian date. SOOO.. I will post a new thread with the updated information.<br /> <br /> .....11/30/07 1042EST.............. i guess it's just a day for mistakes. i was using the file image name rather than the date and time from the header. so, i have to do the dates over again AND THEN convert into julian time. <br /> [END OF DANIELLEYEAGER POST]<br /> <br /> <br /> <br /> --[[User:Spuck|Spuck]] 10:45, 4 December 2007 (PST) Dani, when you write ratio C and ratio D, what do you mean? You are dividing what by what? Also, did you follow the directions from the activity we are working showing you how to generate a light curve. In the activity one of the things you are asked to do is convert to Julian time.<br /> <br /> <br /> --[[User:Danielle|Dani]] 10:49, 4 December 2007 (PST) TSpuck, Ratio C means the Candidate C divided by the average of the references. Ratio D means the Candidate D divided by the average of the references. And no, I did not use the activity worksheet. [end]<br /> <br /> == Perth11/27/07 ==<br /> <br /> Once again the Telescope at perth is not imageing.<br /> nick<br /> <br /> == 11/28/07 ==<br /> <br /> Perth is down again today. Unable to acquire new images. 1308est as well as at 1630est Nick.<br /> <br /> == 11/29/07 ==<br /> <br /> Perth is down again today. Unable to acquire new images. 1318est Nick.<br /> <br /> == Practice Light Curve and Loop Problem ==<br /> <br /> ..............DANIELLEYEAGER 11/30/07 1336EST<br /> <br /> After figuring the Julian Date for the data, the light curve started to loop. By loop, I mean that the dates stacked fairly close to right above one another and circled through them forming a loop. By this loop problem, I've made the assumption that if a set of data has several points that are seconds or minutes apart, the data will loop. To solve the loop problem I averaged together the points that formed the loop and had that as my point. Doing so decreased my data points severely, but did work in achieving my desired goal.<br /> <br /> <br /> NOTE .... when uploading pictures make sure to use EXACT title. example.. if the file name is uploaded as graph2.JPG you must type exactly, example capatalizing the JPG.<br /> <br /> NEW DATA TABLE AND GRAPH<br /> <br /> JULIAN DATE..... RATIO C..... RATIO D<br /> <br /> 2454168.838........ 4.52............ 8.73<br /> <br /> 2454172.835........ 4.386...........6.94<br /> <br /> 2454173.833........ 5.31............ 9.52<br /> <br /> 2454174.84.......... 2.77............ 7.43<br /> <br /> 2454175.835........ 4.21............ 6.36<br /> <br /> [[Image:graph2.JPG]]<br /> <br /> <br /> --[[User:Spuck|Spuck]] 11:03, 4 December 2007 (PST) Dani, Can you double check the last two data points on your graph (2454174.84 and 2454175.835)? The curves seem to match up except for one of these two sets. <br /> <br /> Also, does anyone know how to set up a graph in excel so that you only connect some of the data points being graphed? Thanks.<br /> <br /> [END OF DANIELLYEAGER POST]<br /> <br /> == 11/30/07 practicing posting ==<br /> <br /> .......DANIELLYEAGER..... ALEXISMCCOOL... JENNIFERBUTCHART.... 1509 EST<br /> <br /> <br /> to use an image upload file and then insert using the word Image with a colon after words and then the file name, entire thing surrounded by two closed brackets.<br /> <br /> example. <br /> <br /> [[Image:graph2.JPG]]&lt;br&gt;<br /> [nicks image.] [[Image:Graph3.JPG]]<br /> <br /> bullet points<br /> *one<br /> **two<br /> ***three<br /> <br /> You should be commenting on your progress daily to every other day.<br /> <br /> IF YOU HAVE A QUESTION FOR SOMEONE, USE THE FOLLOWING OR A SIMILAR FORMAT.... PERSON'S NAME---type your question.<br /> <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> <br /> Matt's Light Curve using Beth Thomas's Method<br /> <br /> [[Image:Matt.JPG]]<br /> <br /> HJD YSO 1 in R YSO 1 in I<br /> 2454168 7703 17560<br /> 2454172 7418 17440<br /> 2454173 7869 19369<br /> 2454174 8038 19293<br /> 2454175 7869 19316<br /> 2454177 8565 18534<br /> 2454178 8820 18737<br /> 2454179 8820 19204<br /> 2454180 8820 18871<br /> 2454181 8258 18534<br /> 2454182 7820 18710<br /> 2454182 7708 18729<br /> <br /> == 11/30/07__2257 est ==<br /> <br /> .......DANIELLEYEAGER..........<br /> <br /> Access available from fathers house. Security problem under control. It was because of the http's'... does anyone have any questions about the wiki or the practice light curve? post what you can. if you need to, get ahold of me this weekend. Just a quick reminder that all 25 hours must be completly by Friday December 7th. <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> ....JENNIFERBUTCHART.... 1500EST<br /> <br /> TODAY I HAVE BEEN ON GALAXY ZOO IDENTIFYING GALAXIES. ALSO, I HAVE STARTED WORKING ON NAMING THE .FITS FILES THAT MR. SPUCK GAVE ME. I AM STILL HAVING A LITTLE TROUBLE WITH THE Sb GALAXIES BUT OTHER THAN THAT, EVERYTHING IS OKAY. <br /> <br /> --[[User:Spuck|Spuck]] 11:07, 4 December 2007 (PST) Jennifer, FYI discussions on the Taurus Galaxy project will now take place in a different part of the Wiki. Go to the discussion page off of the [https://coolwiki.ipac.caltech.edu/index.php/Galaxy_Classification Galaxy Clasification Page]. And know you should not have known that at this point :). Thanks.<br /> <br /> [END JENNIFERBUTCHART POST.]<br /> <br /> == 12/02/07_1554 est ==<br /> <br /> ...DANIELLEYEAGER....<br /> <br /> Jennifer, good job on posting, but from now on, please try to open up a new thread unless what you are posting applys directly to the previous post. Did you have any problems posting?<br /> <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> == 12/02/07_1604 est ==<br /> <br /> ....DANIELLEYEAGER......<br /> <br /> Tried to get on perth and take some images. Telescope was in use by perth. I did go into the images we have already taken and saved some of the images titled Daniscandidates to my personal computer. I don't really know what to do with them though. How many pictures do we have that are focused on my center? Should I start getting the data pulled together and working on my real light curve now that I am finished with my practice light curve? Or should I simply focus on mastering the wiki?<br /> <br /> --[[User:Spuck|Spuck]] 11:18, 4 December 2007 (PST) Dani, you're doing a great job with the Wiki. Unfortunately the Perth Telescope is down for now. I just found out today that the RA motor went bad in the mount. I will post more news as I get it. We will probably have to start using New Mexico Skies telescope for our observations. This means being up at 2:00 AM EST ... any volunteers? For now, why don't you focus on working with the rest of the team ... bringing them up to spped on how to access and use the Wiki, as well as working through the Wiki to see what we should focus on in our AAS Poster.<br /> <br /> 1615 est<br /> <br /> While trying to save over my images, when clicked, some files opened to a page showing the picture directly, where as others had a prompt coming up asking whether I wanted to find the image or save the image. Why?<br /> <br /> --[[User:Spuck|Spuck]] 11:18, 4 December 2007 (PST) Dani, I'm not sure. WHy don't you show me this when you have a chance. Thanks.<br /> <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> == 12/2/07_2226 est ==<br /> <br /> ......DANIELLEYEAGER.....<br /> <br /> dumbie me, i went to log on and do some imaging, but then i realised that it was like.. 10 in the morning. so keep in mind when imaging the +12 to +13 hour time difference.<br /> <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> == Highlights of Wiki for Poster at AAS ==<br /> <br /> ....DANIELLEYEAGER 12/03/07 1036 est....<br /> <br /> Newest part of the project = Find 'interesting' or 'important' parts of the wiki to highlight on poster. You can post parts you would like to use in this thread. ''[If you don't remember how to post on a particular thread, you click edit to the left of the heading of the thread you want to post. If you want to start a new thread, scroll to the top and click on the + (plus) sign beside the tab for edit. And as always, if you have questions on the wiki, type my name in caps and then your question.]''<br /> <br /> <br /> <br /> Example / Rough Draft of poster.<br /> <br /> [[Image:Slide1.JPG]]<br /> <br /> [END OF INTRODUCTION, POST BELOW.]<br /> ___________________________________________________________________________<br /> <br /> <br /> .....DANIELLEYEAGER 12/03/07 1253 EST...<br /> <br /> *Basics on the fact that you are working on real research, and at the same time it is an informational, so if you have questions, nice times out of ten, the information is right there for you to get and work with. [Main page.]<br /> <br /> *A lot of time we work with IR and if someone didn’t know what IR is, we have a section specifically noted for that. [Main Page, section 3]<br /> <br /> *Future research project, Galaxy Classifications. <br /> <br /> *Main page section 8.<br /> <br /> *Users Guide on the bottom of the Main Page.<br /> <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> Nick Kelley 12/03/07 1342 est<br /> <br /> *Past T-Tauri work.<br /> <br /> *Things the wiki allows use to do better.<br /> <br /> *Interaction with other students<br /> <br /> *Allows real Scientific work to be done by students.<br /> <br /> --[[User:Spuck|Spuck]] 11:55, 4 December 2007 (PST) These are great ideas ... keep them coming. Also we have a knew location in the WIKI for posting ideas for the 2008 AAS Wiki poster ideas and work items. SO, please post at the [https://coolwiki.ipac.caltech.edu/index.php/Working_area_for_AAS_jan_2008_poster AAS Wiki Poster Page] in the future. Thanks.<br /> <br /> == Practice curve ==<br /> <br /> Nick's light curve, 12/04/07 1:34<br /> <br /> Julian Date Ratio 1 Ratio 2<br /> 2454172.835 4.4 7<br /> 2454173.833 5.3 9.5<br /> 2454174.843 3.6 7.2<br /> 2454175.835 4.2 6.4<br /> <br /> <br /> <br /> [[Image:Graph3.JPG]]<br /> <br /> Once again Perth is down.<br /> <br /> --[[User:Spuck|Spuck]] 11:39, 4 December 2007 (PST) Nick, Perth will probably be down for a bit. See my previous post to Dani. Also, your light curve looks similar to Dani's. That's good and bad. :) Can you check with Dani and answer the following question for me and then post your responses:<br /> <br /> 1. Did the two of you use all the same reference stars?<br /> <br /> 2. Did the two of you use the same software to get the brightness values for your reference stars and YSO candidates?<br /> <br /> Also, I'd like to se you modify your graph a bit. Label the Y axis more clearly (don't just say ratio ... ratio of what?). Also, turn the julian dates (ie. like I had Dani do hers). And use the scatter plot with the line connecting the data points. Also correct your spelling error in the graph title. Thanks.<br /> <br /> --[[User:Nicholas|Nicholas]] 10:36, 6 December 2007 (PST) Well Mr. Spuck Dani walked me through what to do with the Light Curve so it would be understandable why our light curves would be similar. [end]<br /> <br /> --[[User:Danielle|DanielleYeager]] 09:59, 7 December 2007 (PST) 1.) I don't know if we used the same reference stars, but I do know that he used MORE reference stars than I did.<br /> <br /> 2.) I used HOU.<br /> <br /> ==12/3/07_2048 est==<br /> ....JENNIFERBUTCHART....2048EST<br /> <br /> Today, stayed after with Alexis, Danielle, Cale, and Alix in Mr. Spuck's room. Took notes on basics of things for the Austin trip. Parents signed the permission slip and are pleased with the trip. Mom's meeting with Mr. Spuck went well, obviously.<br /> <br /> 2:40-5:10, worked on galaxy research.<br /> <br /> Tomorrow, doing notes on the book Mr. Spuck gave me. <br /> <br /> I officially have my hours as of today. :)<br /> <br /> --[[User:Spuck|Spuck]] 11:29, 4 December 2007 (PST) Jennifer, I'll need to see the log of your hours sometime before friday. Also, why don't you type up the notes from our discussion and get them posted on to the galaxy classification board. You can make the graphics in paint, or draw and scan them in, or use a digital camera to take pics of your notes and upload the graphics. Either way is fine with me.<br /> <br /> [END JENNIFERBUTCHART POST.]<br /> <br /> <br /> <br /> .. DANIELLEYEAGER 12/04/07 ..<br /> <br /> Jennifer, again, good job on posting, but please post in the Galaxy section, if you need a refresher on how to get to it, from the main page go to Future Research Projects and then from there Galaxy then discussion. I beleive that is the route.<br /> <br /> --[[User:Spuck|Spuck]] 11:25, 4 December 2007 (PST) FYI ... here is the link again to the Go to the discussion page off of the [https://coolwiki.ipac.caltech.edu/index.php/Galaxy_Classification Galaxy Clasification Page]. <br /> <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> == 12/04/07 1349 est ==<br /> <br /> '''''UPDATE IN HOW TO POST PLEASE READ'''''<br /> <br /> <br /> --[[User:Danielle|Dani]] 10:53, 4 December 2007 (PST)When posting, rather than typing your name and time, simply click the icon above the Subject/Headling square that looks like a squiggle. It is the second icon from the right. Click that before you start your post, it will post your name date and time for you. and then at the end of the post, simply type [end]<br /> <br /> --[[User:Spuck|Spuck]] 12:08, 4 December 2007 (PST) This is a very useful tool, so please use it. This is what it looks like on your editing screen:<br /> <br /> [[Image:timestamp.jpg]] [end]<br /> <br /> --[[User:Danielle|DanielleYeager]] 07:34, 5 December 2007 (PST) How do you do a screen shot? .. if you go into your preferences and change your 'nickname' it changes what comes up as your name for your signature.[end]<br /> <br /> --[[User:Nicholas|NicholasJamesKelley]] 10:17, 7 December 2007 (PST) Perth is down at the moment and has been for a couple of days and will continue to be for an indefinite period of time. This is a very depressing bit of info because it not only sets back the spitzer project as a whole but also sets back my and other individual's projects for the Pittsburgh Regional Science and Engineering Fair.<br /> <br /> == Light Curve Correction ==<br /> <br /> --[[User:Danielle|DanielleYeager]] 10:44, 7 December 2007 (PST) In study of both Nick's and my own light curve, we have discovered why the peaks are not matching up. The graphs show two different candidates rather than two different filters for the same candidate. Both light curves need redone, focusing on one candidate in both the I and the R filters. Each graph needs to show the I and R light curve for one candidate. [end]<br /> <br /> --[[User:Nicholas|NicholasJamesKelley]] 10:47, 7 December 2007 (PST) These are my light curves for the 2 candidates that I am monitoring for Spitzer and the Sceince fair. I am currently monitoring to get more accurate curves to take with me.<br /> <br /> <br /> <br /> Candidate <br /> 415 Julian Date I Ratio R Ratio<br /> 12-Feb 2454144.168 1.20 <br /> 21-Feb 2454153.051 1.32 0.6<br /> 22-Feb 2454154.144 1.6 0.63<br /> 23-Feb 2454155.121 1.76 0.84<br /> 27-Feb 2454158.9 1.27 0.53<br /> 6-Mar 2454166.035 1.33 0.56<br /> 9-Mar 2454169.047 1.66 0.73<br /> 11-Mar 2454171.074 1.49 0.68<br /> 12-Mar 2454172.013 1.5 0.65<br /> 16-Mar 2454176.01 0.96 0.45<br /> <br /> [[Image:415.JPG]]<br /> <br /> Candidate <br /> 416 Julian Date I ratio R ratio<br /> 12-Feb 2454144.168 3 <br /> 21-Feb 2454153.051 3.04 1.3<br /> 22-Feb 2454154.144 3.06 1.19<br /> 23-Feb 2454155.121 2.86 1.31<br /> 27-Feb 2454158.9 3.24 1.4<br /> 6-Mar 2454166.035 3.26 1.52<br /> 9-Mar 2454169.047 3.07 1.31<br /> 11-Mar 2454171.074 3.07 1.33<br /> 12-Mar 2454172.013 3.36 1.44<br /> 16-Mar 2454176.01 3.2 1.38<br /> <br /> [[Image:416.JPG]]</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:Working_area_for_AAS_jan_2008_poster&diff=2702 Talk:Working area for AAS jan 2008 poster 2007-12-08T01:39:36Z <p>Mattw: /* Highlights for Galaxy Poster */</p> <hr /> <div>== Front Page Information ==<br /> <br /> --[[User:Danielle|DanielleYeager]] 07:50, 5 December 2007 (PST) As of now, I have a very short and simple statement on the front page of this area of the wiki. If you don't know what I mean, I mean the article section for 'Working area for AAS jan 2008 poster'... Who all is going to be presenting it? What exactly is the abstract? What information to we currently have that I can post out on the main/article page. [end]<br /> <br /> --[[User:Rebull|Rebull]] 14:25, 5 December 2007 (PST) Hi Danielle - I just went ahead and updated it. [end]<br /> <br /> <br /> --[[User:Danielle|DanielleYeager]] 07:24, 6 December 2007 (PST) Thank you very much! [end]<br /> <br /> == Highlights for Wiki AAS Poster ==<br /> <br /> --[[User:Danielle|Dani]] 07:19, 5 December 2007 (PST) this is just copied and pasted over from the IC 2118 thread.<br /> <br /> <br /> <br /> ....DANIELLEYEAGER 12/03/07 1036 est....<br /> <br /> Newest part of the project = Find 'interesting' or 'important' parts of the wiki to highlight on poster. You can post parts you would like to use in this thread. ''[If you don't remember how to post on a particular thread, you click edit to the left of the heading of the thread you want to post. If you want to start a new thread, scroll to the top and click on the + (plus) sign beside the tab for edit. And as always, if you have questions on the wiki, type my name in caps and then your question.]''<br /> <br /> <br /> <br /> Example / Rough Draft of poster.<br /> <br /> [[Image:Slide1.JPG]]<br /> <br /> [END OF INTRODUCTION, POST BELOW.]<br /> ___________________________________________________________________________<br /> <br /> <br /> .....DANIELLEYEAGER 12/03/07 1253 EST...<br /> <br /> *Basics on the fact that you are working on real research, and at the same time it is an informational, so if you have questions, nine times out of ten, the information is right there for you to get and work with. [Main page.]<br /> <br /> *A lot of time we work with IR and if someone didn’t know what IR is, we have a section specifically noted for that. [Main Page, section 3]<br /> <br /> *Future research project, Galaxy Classifications. <br /> <br /> *Main page section 8.<br /> <br /> *Users Guide on the bottom of the Main Page.<br /> <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> Nick Kelley 12/03/07 1342 est<br /> <br /> *Past T-Tauri work.<br /> <br /> *Things the wiki allows use to do better.<br /> <br /> *Interaction with other students<br /> <br /> *Allows real Scientific work to be done by students.<br /> <br /> --[[User:Spuck|Spuck]] 11:55, 4 December 2007 (PST) These are great ideas ... keep them coming. Also we have a knew location in the WIKI for posting ideas for the 2008 AAS Wiki poster ideas and work items. SO, please post at the [https://coolwiki.ipac.caltech.edu/index.php/Working_area_for_AAS_jan_2008_poster AAS Wiki Poster Page] in the future. Thanks.<br /> <br /> <br /> --[[User:Danielle|DanielleYeager]] 10:48, 5 December 2007 (PST) <br /> *Finding cluster members<br /> <br /> *The playground<br /> <br /> *How can I find already-reduced Spitzer data?<br /> <br /> <br /> <br /> --[[User:Nicholas|NicholasJamesKelley]] 10:40, 6 December 2007 (PST) It would also be very nice if other people contributed to Ideas.<br /> <br /> --[[User:Danielle|DanielleYeager]] 10:06, 7 December 2007 (PST) Yes, Nick, it would be nice if other people contributed, but until they do, it's important that we continue to research and post. The most important feature is that a non-user[meaning, someone without a user name and password to the page] can get more information from the site than they more than likely know what to do with and the fact that the authors are talking 'behind the scenes', what we know as the discusion sections, and the site evolves and shifts as the projects progress.<br /> <br /> == Highlights for Galaxy Poster ==<br /> Researchers and presenters for the galaxy project include Cale McClintock, Jennifer Butchart, Alexis McCool and Alix Holcomb.<br /> The poster will be presented at the upcoming AAS meeting in Austin Texas.<br /> <br /> == Highlights for WZ Sge Poster ==<br /> <br /> WZSge is an eclipsing binary star system composed of a white dwarf(serving as the primary star) and a brown dwarf(which serves as a secondary star). This is a close orbital binary star system with only an 82 minute orbital period. What is happening in WZSge is the white dwarf is stripping material away from the brown dwarf, however due to angular momentum the material is not falling directly into the white dwarf it is falling into an accretion disk which surrounds the white dwarf. This accrection disk is so bright that when WZSge is imaged in the optical we are not actually seeing the white dwarf but in fact the accretion disk which surrounds it. In the optical we can see by generating a light curve that the brown dwarf eclipses in front of the white dwarf and its accretion disk. However the current phenomena of WZSge is that an eclipse is visible in the IR (at both 4.5 and 8 microns).<br /> <br /> Researchers for this project include:<br /> Steve Howell NOAO WIYN, Don Hoard SSC Harvey Mudd, J.M. Santiago and Jeff Adkins Deer Valley High School, Kimmerly Johnson and Beth Thomas, Matt Walentosky and Tim Spuck Oil City High School.<br /> <br /> The poster &quot;WZSge: Dark Matter in Accretion Disks&quot; will be presented at the 211th annual meeting of the American Astronomical Society in Austin Texas this coming January.</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:Working_area_for_AAS_jan_2008_poster&diff=2701 Talk:Working area for AAS jan 2008 poster 2007-12-08T01:37:13Z <p>Mattw: /* Highlights for WZ Sge Poster */</p> <hr /> <div>== Front Page Information ==<br /> <br /> --[[User:Danielle|DanielleYeager]] 07:50, 5 December 2007 (PST) As of now, I have a very short and simple statement on the front page of this area of the wiki. If you don't know what I mean, I mean the article section for 'Working area for AAS jan 2008 poster'... Who all is going to be presenting it? What exactly is the abstract? What information to we currently have that I can post out on the main/article page. [end]<br /> <br /> --[[User:Rebull|Rebull]] 14:25, 5 December 2007 (PST) Hi Danielle - I just went ahead and updated it. [end]<br /> <br /> <br /> --[[User:Danielle|DanielleYeager]] 07:24, 6 December 2007 (PST) Thank you very much! [end]<br /> <br /> == Highlights for Wiki AAS Poster ==<br /> <br /> --[[User:Danielle|Dani]] 07:19, 5 December 2007 (PST) this is just copied and pasted over from the IC 2118 thread.<br /> <br /> <br /> <br /> ....DANIELLEYEAGER 12/03/07 1036 est....<br /> <br /> Newest part of the project = Find 'interesting' or 'important' parts of the wiki to highlight on poster. You can post parts you would like to use in this thread. ''[If you don't remember how to post on a particular thread, you click edit to the left of the heading of the thread you want to post. If you want to start a new thread, scroll to the top and click on the + (plus) sign beside the tab for edit. And as always, if you have questions on the wiki, type my name in caps and then your question.]''<br /> <br /> <br /> <br /> Example / Rough Draft of poster.<br /> <br /> [[Image:Slide1.JPG]]<br /> <br /> [END OF INTRODUCTION, POST BELOW.]<br /> ___________________________________________________________________________<br /> <br /> <br /> .....DANIELLEYEAGER 12/03/07 1253 EST...<br /> <br /> *Basics on the fact that you are working on real research, and at the same time it is an informational, so if you have questions, nine times out of ten, the information is right there for you to get and work with. [Main page.]<br /> <br /> *A lot of time we work with IR and if someone didn’t know what IR is, we have a section specifically noted for that. [Main Page, section 3]<br /> <br /> *Future research project, Galaxy Classifications. <br /> <br /> *Main page section 8.<br /> <br /> *Users Guide on the bottom of the Main Page.<br /> <br /> [END OF DANIELLEYEAGER POST.]<br /> <br /> Nick Kelley 12/03/07 1342 est<br /> <br /> *Past T-Tauri work.<br /> <br /> *Things the wiki allows use to do better.<br /> <br /> *Interaction with other students<br /> <br /> *Allows real Scientific work to be done by students.<br /> <br /> --[[User:Spuck|Spuck]] 11:55, 4 December 2007 (PST) These are great ideas ... keep them coming. Also we have a knew location in the WIKI for posting ideas for the 2008 AAS Wiki poster ideas and work items. SO, please post at the [https://coolwiki.ipac.caltech.edu/index.php/Working_area_for_AAS_jan_2008_poster AAS Wiki Poster Page] in the future. Thanks.<br /> <br /> <br /> --[[User:Danielle|DanielleYeager]] 10:48, 5 December 2007 (PST) <br /> *Finding cluster members<br /> <br /> *The playground<br /> <br /> *How can I find already-reduced Spitzer data?<br /> <br /> <br /> <br /> --[[User:Nicholas|NicholasJamesKelley]] 10:40, 6 December 2007 (PST) It would also be very nice if other people contributed to Ideas.<br /> <br /> --[[User:Danielle|DanielleYeager]] 10:06, 7 December 2007 (PST) Yes, Nick, it would be nice if other people contributed, but until they do, it's important that we continue to research and post. The most important feature is that a non-user[meaning, someone without a user name and password to the page] can get more information from the site than they more than likely know what to do with and the fact that the authors are talking 'behind the scenes', what we know as the discusion sections, and the site evolves and shifts as the projects progress.<br /> <br /> == Highlights for Galaxy Poster ==<br /> <br /> asdfgswfsdfg<br /> <br /> == Highlights for WZ Sge Poster ==<br /> <br /> WZSge is an eclipsing binary star system composed of a white dwarf(serving as the primary star) and a brown dwarf(which serves as a secondary star). This is a close orbital binary star system with only an 82 minute orbital period. What is happening in WZSge is the white dwarf is stripping material away from the brown dwarf, however due to angular momentum the material is not falling directly into the white dwarf it is falling into an accretion disk which surrounds the white dwarf. This accrection disk is so bright that when WZSge is imaged in the optical we are not actually seeing the white dwarf but in fact the accretion disk which surrounds it. In the optical we can see by generating a light curve that the brown dwarf eclipses in front of the white dwarf and its accretion disk. However the current phenomena of WZSge is that an eclipse is visible in the IR (at both 4.5 and 8 microns).<br /> <br /> Researchers for this project include:<br /> Steve Howell NOAO WIYN, Don Hoard SSC Harvey Mudd, J.M. Santiago and Jeff Adkins Deer Valley High School, Kimmerly Johnson and Beth Thomas, Matt Walentosky and Tim Spuck Oil City High School.<br /> <br /> The poster &quot;WZSge: Dark Matter in Accretion Disks&quot; will be presented at the 211th annual meeting of the American Astronomical Society in Austin Texas this coming January.</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=File:Dick_cheney.jpg&diff=2304 File:Dick cheney.jpg 2007-08-01T18:46:52Z <p>Mattw: </p> <hr /> <div></div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=IC_2118_Current_Research_Activities&diff=2152 IC 2118 Current Research Activities 2007-07-23T21:27:51Z <p>Mattw: /* T-Tauri/IC2118 Presentation for Astroblast 2007 */</p> <hr /> <div>== [[Writing the Research Paper for IC2118]] ==<br /> <br /> <br /> == [[Information for Oil City High School meetings]] ==<br /> <br /> The next meeting should be at 4 0'clock pm wednesday the 25th at matt walentosky's house. (Specifically for people going to California, so we can plan out events and travel...)<br /> <br /> == Proposal for Radio Observations of T-Tauri Candidates in IC2118 == <br /> <br /> <br /> '''''SUPPORT INFORMATION - T-Tauri Candidates Emit Radio'''''<br /> <br /> '''FROM MATT WALENTOSKY 6/30/2007 @ 2:30 PM - Two Abstracts Below'''<br /> <br /> Title: Radio emission from pre-main-sequence stars<br /> Authors: Skinner, Stephen Lee<br /> <br /> Affiliation: AA(Colorado Univ., Boulder.)<br /> Publication: Ph.D. Thesis Colorado Univ., Boulder.<br /> Publication Date: 01/1992<br /> Category: Space Radiation<br /> Origin: STI<br /> <br /> Abstract<br /> This study focuses on the properties and physical origin of radio continuum emission from pre-main-sequence (PMS) stars. These are young stars, typically less than a few million years old, and are still in a phase of gravitational contraction that will ultimately be halted by the onset of hydrogen burning in their cores. First, I address the question of the origin of centimeter continuum emission in intermediate mass (approx. equal to 3-20 solar mass) PMS stars, the so-called 'Herbig Ae/Be stars'. A high-sensitivity radio survey of 57 such stars was undertaken using the Very Large Array and Australia Telescope, resulting in the detection of twelve stars. These observations provide a homogenous data base consisting of information on source sizes, radio luminosities, variability timescales, circular polarization, and spectral energy distributions in the wavelength range 2-20 cm. Using these data along with previously published spectroscopy, I conclude that centimeter radio emission from Herbig Ae/Be stars is predominantly thermal and in many cases wind-related. An unexpected result of the above program was the serendipitous detection of circularly polarized radio emission in the low mass (approx. equal to 1 solar mass) PMS star Hubble 4, a member of the class of 'weak-lined T Tauri stars' (WTTS). This provides some of the most convincing evidence to date for the existence of ordered magnetic fields in WTTS. In a second observing program, I have searched for evidence of cold (less than or equal to 50 K) circumstellar dust around WTTS, which might exist in the form of remnant disks. Of the sixteen WTTS that were observed in the wavelength range 450-1100 microns using the James Clerk Maxwell Telescope, only V836 Tau was detected. Its spectral energy distribution longward of 10 microns is consistent with that expected for a flat, axisymmetric circumstellar disk of mass approx. equal to 0.04 solar mass (= 42 Jupiter masses). This star may be a rare example of an object in which disk dispersal is underway, but not yet complete.<br /> <br /> <br /> Title: Centimeter Radio Emission from Low-Mass Weak T Tauri Stars in Taurus-Auriga<br /> Authors: Chiang, Eugene; Phillips, R. B.<br /> <br /> Affiliation: AA(MIT), AB(MIT Haystack Observatory)<br /> Publication: American Astronomical Society, 185th AAS Meeting, #48.08; Bulletin of the American Astronomical Society, Vol. 26, p.1388<br /> Publication Date: 12/1994<br /> Origin: AAS<br /> Abstract Copyright:(c) 1994: American Astronomical Society<br /> <br /> Abstract<br /> We report on the results of a sensitive survey for lambda 3.6 cm radio emission from low-mass, weak T Tauri (WTT) stars in the Taurus-Auriga cloud complex. The target population consists of stars in the Herbig and Bell Catalog of spectral type K7 or later, and W(Hα ) &lt;= 10 Angstroms. Of the 28 such stars surveyed using the Very Large Array down to detection thresholds of ~ 0.1 mJy, 7 (possibly 8) are observed to emit at strengths ranging from 0.1 to 2 mJy. Five of these young radio stars are newly discovered in our survey: V827 Tau and V710 Tau B are discovered to be relatively strong sources of mJy emission, while IW Tau, UX Tau B, and the possible detection LkHa 332-G1 form a new population of relatively weak emitters. Our radio survey and complementary surveys are pooled, and of 43 WTT stars K7 or later in Tau-Aur, 14 are now known to be radio emitters at lambda 6 and lambda 3.6 cm. Correlations between radio luminosity and other stellar parameters have been attempted but generally yield null results. Wide binarity (component separations in excess of 0''.13, 20 AU) appears unrelated to radio emission, as does spectral type. Furthermore, we find no convincing evidence for the extreme youth of radio stars, contrary to claims in the literature over the past decade. While we do find that radio-loud stars in our sample are formally younger than the radio-quiet stars by about 0.5 Myr, the reality of this relatively small age difference is highly suspect given uncertainties in the placement of these stars on the HR diagram. Moreover, Monte Carlo-type calculations involving distributing the stars on both the HR diagram and local CO gas density cast doubts on any differences between the radio stars and the general WTT population. We conclude that the age effect for low-mass radio WTT stars in Tau-Aur, if real, is much smaller than previous estimations by factors of 4-10. It is also possible centimeter wavelength surveys to date have still not properly described the radio luminosity function of low-mass WTT stars in Tau-Aur, and we urge future observations of these young stars with denser temporal coverage.<br /> <br /> '''FROM SPUCK 6/30/2007 @ 2:35pm'''<br /> <br /> I'm not sure that we will be able to use the GBT telescope in Green Bank for observations. The beamwidth at 10-15 GHz is probably too big.<br /> <br /> Here are the specs for the GBT<br /> Beamwidth (Table 3) Diffraction beamwidth (FWHM)<br /> 8 GHz it is 90&quot;, <br /> 20 GHz it is 36&quot;, <br /> 50 GHz it is 14&quot;<br /> <br /> Here are some questions from Sue Ann Heatherly at NRAO-Green Bank - One question I have is: is the resolving<br /> power of the GBT sufficient to distinguish spatially between individual stars? Does large scale emission exist within the nebula that will confuse your results?<br /> <br /> The VLA is probably the only instrument that can be used.<br /> <br /> Synthesized Beamwidth (arcsec)depending on configuration<br /> '''Nick Kelley 6/30/2007 3:00PM''' <br /> <br /> 400 cm 24.0&quot; 80.0&quot; 260.0&quot; 850.0&quot;<br /> <br /> 90 cm 6.0&quot; 17.0&quot; 56.0&quot; 200.0&quot; <br /> <br /> 20 cm 1.4 &quot; 3.9&quot; 12.5&quot; 44.0&quot; <br /> <br /> 6 cm 0.4 &quot; 1.2&quot;&quot;&quot; 3.9 &quot; 14.0 &quot;<br /> <br /> 3.6 cm 0.24 &quot; 0.7&quot; 2.3 &quot; 8.4 &quot;<br /> <br /> 2 cm 0.14 &quot; 0.4 &quot; 1.2&quot; 3.9&quot;<br /> <br /> 1.3 cm 0.08 &quot; 0.3&quot; 0.9 &quot;2.8&quot; <br /> <br /> 0.7 cm 0.05 0.15 0.47 1<br /> restricting my creativity<br /> <br /> == T-Tauri/IC2118 Presentation for Astroblast 2007 ==<br /> <br /> '''''Oil City High School students will be presenting August 11 at the Oil Region Astronomical Observatory'''''<br /> <br /> <br /> <br /> FROM Nicholas James Kelley <br /> <br /> Astroblast is amazin ... see pic<br /> <br /> [[Image: astroblast1.JPG|center]]<br /> <br /> Is their anyway we can attach the powerpoint here?? Matt W.<br /> <br /> == Monitoring T-Tauri Stars using the Perth Obervatory Telescope ==<br /> <br /> '''Generating Light Curves'''<br /> <br /> Using Perth Telescope<br /> <br /> 1. Check to see what the current sky conditions are by checking the live camera<br /> <br /> http://www.perthobservatory.wa.gov.au//information/po_sky_camera.html<br /> <br /> 2. Check to see what the current weather conditions are<br /> <br /> http://www.perthobservatory.wa.gov.au//information/po_weather.html<br /> <br /> 3. Weather forecast for Perth - http://www.bom.gov.au/weather/wa/<br /> <br /> Log into telescope if conditions look good.<br /> <br /> http://perthobservatory.org or http://202.72.190.15<br /> <br /> EMAIL tspuck@hotmail.com for telescope access<br /> <br /> == Chandra X-Ray Data ==<br /> <br /> '''''To date no X-Ray data for IC2118 has been located.''''' If you know of any please contact Tim Spuck at tspuck@hotmail.com.<br /> <br /> == Kitt Peak H-alpha Data ==<br /> <br /> '''''In January of 2007 students from Oil City High School used the 0.9 Meter Telescope at Kitt peak to image regions of IC2118 in H-alpha.''''<br /> <br /> Matt Walentosky, Nick Kelley, Sandy Weiser were the students who went!!!!!!<br /> <br /> == USNO U, B, V, R, and I Data ==<br /> <br /> '''''U, B, V, R, and I data will be used to generate more accurate SEDs for the T-Tauri Candidates'''''<br /> <br /> == Outflows or Jets ==<br /> <br /> '''''Visible outflows or jets are strong evidence that a candidate is indeed a T-Tauri Star'''''<br /> <br /> <br /> <br /> == Multi Wavelength Composite Images ==<br /> <br /> '''''Images and Methods'''''<br /> <br /> FROM SPUCK 6/30/2007 See Image Below- IC 2118 3.6 µm (blue), 5.8 µm (green), 8.0 µm (red) tri-color composite generated using MaxIm DL. (By M. Heath, N. Kelley, P. Morton, M. Walentosky, S. Weiser – Oil City High School, Oil City, PA)<br /> <br /> [[Image: spuckim3.JPG|center]]</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=IC_2118_Current_Research_Activities&diff=2147 IC 2118 Current Research Activities 2007-07-23T21:20:19Z <p>Mattw: /* Information for Oil City High School meetings */</p> <hr /> <div>== [[Writing the Research Paper for IC2118]] ==<br /> <br /> <br /> == [[Information for Oil City High School meetings]] ==<br /> <br /> The next meeting should be at 4 0'clock pm wednesday the 25th at matt walentosky's house. (Specifically for people going to California, so we can plan out events and travel...)<br /> <br /> == Proposal for Radio Observations of T-Tauri Candidates in IC2118 == <br /> <br /> <br /> '''''SUPPORT INFORMATION - T-Tauri Candidates Emit Radio'''''<br /> <br /> '''FROM MATT WALENTOSKY 6/30/2007 @ 2:30 PM - Two Abstracts Below'''<br /> <br /> Title: Radio emission from pre-main-sequence stars<br /> Authors: Skinner, Stephen Lee<br /> <br /> Affiliation: AA(Colorado Univ., Boulder.)<br /> Publication: Ph.D. Thesis Colorado Univ., Boulder.<br /> Publication Date: 01/1992<br /> Category: Space Radiation<br /> Origin: STI<br /> <br /> Abstract<br /> This study focuses on the properties and physical origin of radio continuum emission from pre-main-sequence (PMS) stars. These are young stars, typically less than a few million years old, and are still in a phase of gravitational contraction that will ultimately be halted by the onset of hydrogen burning in their cores. First, I address the question of the origin of centimeter continuum emission in intermediate mass (approx. equal to 3-20 solar mass) PMS stars, the so-called 'Herbig Ae/Be stars'. A high-sensitivity radio survey of 57 such stars was undertaken using the Very Large Array and Australia Telescope, resulting in the detection of twelve stars. These observations provide a homogenous data base consisting of information on source sizes, radio luminosities, variability timescales, circular polarization, and spectral energy distributions in the wavelength range 2-20 cm. Using these data along with previously published spectroscopy, I conclude that centimeter radio emission from Herbig Ae/Be stars is predominantly thermal and in many cases wind-related. An unexpected result of the above program was the serendipitous detection of circularly polarized radio emission in the low mass (approx. equal to 1 solar mass) PMS star Hubble 4, a member of the class of 'weak-lined T Tauri stars' (WTTS). This provides some of the most convincing evidence to date for the existence of ordered magnetic fields in WTTS. In a second observing program, I have searched for evidence of cold (less than or equal to 50 K) circumstellar dust around WTTS, which might exist in the form of remnant disks. Of the sixteen WTTS that were observed in the wavelength range 450-1100 microns using the James Clerk Maxwell Telescope, only V836 Tau was detected. Its spectral energy distribution longward of 10 microns is consistent with that expected for a flat, axisymmetric circumstellar disk of mass approx. equal to 0.04 solar mass (= 42 Jupiter masses). This star may be a rare example of an object in which disk dispersal is underway, but not yet complete.<br /> <br /> <br /> Title: Centimeter Radio Emission from Low-Mass Weak T Tauri Stars in Taurus-Auriga<br /> Authors: Chiang, Eugene; Phillips, R. B.<br /> <br /> Affiliation: AA(MIT), AB(MIT Haystack Observatory)<br /> Publication: American Astronomical Society, 185th AAS Meeting, #48.08; Bulletin of the American Astronomical Society, Vol. 26, p.1388<br /> Publication Date: 12/1994<br /> Origin: AAS<br /> Abstract Copyright:(c) 1994: American Astronomical Society<br /> <br /> Abstract<br /> We report on the results of a sensitive survey for lambda 3.6 cm radio emission from low-mass, weak T Tauri (WTT) stars in the Taurus-Auriga cloud complex. The target population consists of stars in the Herbig and Bell Catalog of spectral type K7 or later, and W(Hα ) &lt;= 10 Angstroms. Of the 28 such stars surveyed using the Very Large Array down to detection thresholds of ~ 0.1 mJy, 7 (possibly 8) are observed to emit at strengths ranging from 0.1 to 2 mJy. Five of these young radio stars are newly discovered in our survey: V827 Tau and V710 Tau B are discovered to be relatively strong sources of mJy emission, while IW Tau, UX Tau B, and the possible detection LkHa 332-G1 form a new population of relatively weak emitters. Our radio survey and complementary surveys are pooled, and of 43 WTT stars K7 or later in Tau-Aur, 14 are now known to be radio emitters at lambda 6 and lambda 3.6 cm. Correlations between radio luminosity and other stellar parameters have been attempted but generally yield null results. Wide binarity (component separations in excess of 0''.13, 20 AU) appears unrelated to radio emission, as does spectral type. Furthermore, we find no convincing evidence for the extreme youth of radio stars, contrary to claims in the literature over the past decade. While we do find that radio-loud stars in our sample are formally younger than the radio-quiet stars by about 0.5 Myr, the reality of this relatively small age difference is highly suspect given uncertainties in the placement of these stars on the HR diagram. Moreover, Monte Carlo-type calculations involving distributing the stars on both the HR diagram and local CO gas density cast doubts on any differences between the radio stars and the general WTT population. We conclude that the age effect for low-mass radio WTT stars in Tau-Aur, if real, is much smaller than previous estimations by factors of 4-10. It is also possible centimeter wavelength surveys to date have still not properly described the radio luminosity function of low-mass WTT stars in Tau-Aur, and we urge future observations of these young stars with denser temporal coverage.<br /> <br /> '''FROM SPUCK 6/30/2007 @ 2:35pm'''<br /> <br /> I'm not sure that we will be able to use the GBT telescope in Green Bank for observations. The beamwidth at 10-15 GHz is probably too big.<br /> <br /> Here are the specs for the GBT<br /> Beamwidth (Table 3) Diffraction beamwidth (FWHM)<br /> 8 GHz it is 90&quot;, <br /> 20 GHz it is 36&quot;, <br /> 50 GHz it is 14&quot;<br /> <br /> Here are some questions from Sue Ann Heatherly at NRAO-Green Bank - One question I have is: is the resolving<br /> power of the GBT sufficient to distinguish spatially between individual stars? Does large scale emission exist within the nebula that will confuse your results?<br /> <br /> The VLA is probably the only instrument that can be used.<br /> <br /> Synthesized Beamwidth (arcsec)depending on configuration<br /> '''Nick Kelley 6/30/2007 3:00PM''' <br /> <br /> 400 cm 24.0&quot; 80.0&quot; 260.0&quot; 850.0&quot;<br /> <br /> 90 cm 6.0&quot; 17.0&quot; 56.0&quot; 200.0&quot; <br /> <br /> 20 cm 1.4 &quot; 3.9&quot; 12.5&quot; 44.0&quot; <br /> <br /> 6 cm 0.4 &quot; 1.2&quot;&quot;&quot; 3.9 &quot; 14.0 &quot;<br /> <br /> 3.6 cm 0.24 &quot; 0.7&quot; 2.3 &quot; 8.4 &quot;<br /> <br /> 2 cm 0.14 &quot; 0.4 &quot; 1.2&quot; 3.9&quot;<br /> <br /> 1.3 cm 0.08 &quot; 0.3&quot; 0.9 &quot;2.8&quot; <br /> <br /> 0.7 cm 0.05 0.15 0.47 1<br /> restricting my creativity<br /> <br /> == T-Tauri/IC2118 Presentation for Astroblast 2007 ==<br /> <br /> '''''Oil City High School students will be presenting August 11 at the Oil Region Astronomical Observatory'''''<br /> <br /> <br /> <br /> FROM Nicholas James Kelley <br /> <br /> Astroblast is amazin ... see pic<br /> <br /> [[Image: astroblast1.JPG|center]]<br /> <br /> == Monitoring T-Tauri Stars using the Perth Obervatory Telescope ==<br /> <br /> '''Generating Light Curves'''<br /> <br /> Using Perth Telescope<br /> <br /> 1. Check to see what the current sky conditions are by checking the live camera<br /> <br /> http://www.perthobservatory.wa.gov.au//information/po_sky_camera.html<br /> <br /> 2. Check to see what the current weather conditions are<br /> <br /> http://www.perthobservatory.wa.gov.au//information/po_weather.html<br /> <br /> 3. Weather forecast for Perth - http://www.bom.gov.au/weather/wa/<br /> <br /> Log into telescope if conditions look good.<br /> <br /> http://perthobservatory.org or http://202.72.190.15<br /> <br /> EMAIL tspuck@hotmail.com for telescope access<br /> <br /> == Chandra X-Ray Data ==<br /> <br /> '''''To date no X-Ray data for IC2118 has been located.''''' If you know of any please contact Tim Spuck at tspuck@hotmail.com.<br /> <br /> == Kitt Peak H-alpha Data ==<br /> <br /> '''''In January of 2007 students from Oil City High School used the 0.9 Meter Telescope at Kitt peak to image regions of IC2118 in H-alpha.''''<br /> <br /> Matt Walentosky, Nick Kelley, Sandy Weiser were the students who went!!!!!!<br /> <br /> == USNO U, B, V, R, and I Data ==<br /> <br /> '''''U, B, V, R, and I data will be used to generate more accurate SEDs for the T-Tauri Candidates'''''<br /> <br /> == Outflows or Jets ==<br /> <br /> '''''Visible outflows or jets are strong evidence that a candidate is indeed a T-Tauri Star'''''<br /> <br /> <br /> <br /> == Multi Wavelength Composite Images ==<br /> <br /> '''''Images and Methods'''''<br /> <br /> FROM SPUCK 6/30/2007 See Image Below- IC 2118 3.6 µm (blue), 5.8 µm (green), 8.0 µm (red) tri-color composite generated using MaxIm DL. (By M. Heath, N. Kelley, P. Morton, M. Walentosky, S. Weiser – Oil City High School, Oil City, PA)<br /> <br /> [[Image: spuckim3.JPG|center]]</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:Main_Page&diff=1852 Talk:Main Page 2007-06-30T19:57:24Z <p>Mattw: /* Kitt Peak H-alpha Data */</p> <hr /> <div>== Planning for work session June 29 and/or June 30th for Oil City Students ==<br /> <br /> Matt, Matt, Nick, Greg, Danni, Alexis, and Sandy,<br /> <br /> We had tentatively planned to meet to work on Spitzer stuff and get ready for California on Friday June 29 and/or Saturday June 30. We could meet at the high school something that might be a bit more relaxed is to meet here at my house near Pine City. Please make comments here at the Wiki site as to what your schedule is like and whether or not you can make a work session. Please do this ASAP so we can decide what will work.<br /> <br /> Thanks, Mr. Spuck<br /> <br /> Anytime on Saturday the 30th is good for me. I can not make it on the 29th because my brother is arriving from New Jersey that day. Where exactly in Pine City do you live? Could you send directions to my email? Matt H.<br /> <br /> FROM SPUCK - <br /> - Turn LEFT onto E 1ST ST / US-62 N. Continue to follow US-62 N. Go 2.9 miles Map <br /> <br /> - US-62 N becomes PA-157. Go 13.5 miles Map <br /> <br /> - Turn SLIGHT RIGHT onto PA-208. Go 3.7 miles Map <br /> <br /> - Turn RIGHT onto MILLERSTOWN RD. Go 1.4 miles <br /> <br /> - Gravel lane is on right hand side. Come up lane about 1000 feet.<br /> <br /> [[Image: directions.JPG|center]]<br /> <br /> <br /> <br /> How late into saturday are you planning to work saturday b/c i can't be there until like 1 o'clock earliest!! MATT W.<br /> <br /> FROM SPUCK - Is there another day that works better for everyone ... for example Monday morning July 2 into MOnday afternoon??? Please let me know what your schedule is. Also, keep in mind when you make comments that this discussion page is something that can be viewed by the entire world. This is ok, because we want other teacher/student research teams to see first hand the both the good and bad of trying to conduct student teacher research. We are kind of like the &quot;reality TV show&quot; only on the web. :) Thanks, please respond ASAP. Mr. Spuck<br /> <br /> I am gonna be gone from the July 1st to the 6th in Virginia. I was talking to Nick Kelley and he was saying that he can make it on the 30th anytime like me. Whatever time Matt W. can make the meeting is fine with me and Nick!! Also Greg is currently in Washington DC with a biology seminar and will not be back till July 3rd. He wanted me to fill him in with all the info he is gonna miss when he gets back. Matt H.<br /> <br /> FROM SPUCK - Ok ... it looks like we will meet on Saturday (June 30th). Has anyone spoken to Danni or Alexis?? So where do we want to meet and what time? I'm not sure what condition my room is at the high school because of summer cleaning. I will know more tomorrow when I go up to the school. If we meet at my place, I think we should start BY 10:00 AM and plan on going till about 5:00 PM. If your parents could bring you out, then I could get you back to the Oil City area by 6:00 PM on Saturday, or they can pick you up. Let me know what you think. Matt H. ... have you been in recent contact with Nick? Why has he not posted on the Wiki? Thanks.<br /> <br /> I have been talking to Nick about our upcoming meeting this weekend. However right now Nick is grounded and I believe he can not use the internet.(not sure totally) Also that time at your house is fine with me. Though I might have to be leaving an hour early but right now I'm not certain, I will find out tomorrow and post it up here. Also I will try to get a hold of Nick to tell him about the meeting. Matt H.<br /> <br /> SaturdaY IS THE BEST DAy for me i work 11pm to 7am sundaye night and i work 11pm 7am monday night so that wont work<br /> <br /> FROM SPUCK - I'll assume the comments above are from Nick Kelley. I'f wrong please let me know. I checked my room out yesterday at the high school and everything has been removed for cleaning. So I guess it is my house (see directions above). Plan on arriving between 9:30 and 10:00 AM and we will plan on stopping right around 5:00 PM. Either your parents could pick you up at 5:00 PM or I'll be going to Oil City around 6:00 PM on Saturday and I could give you a ride. If I have this correct it will be Nick at Matt H, with Matt W coming by in the afternoon. Anyone else?<br /> <br /> Sounds right to me... Matt W.<br /> <br /> DANI- account up and running. w00o<br /> <br /> FROM SPUCK - Dani, Matt H, Matt W, and Nick K met and worked on the following:<br /> Using the Perth Telescope,<br /> Radio Proposal,<br /> Wiki Discussion Links,<br /> WZ Sge Observations,<br /> Review of Luisa's Tutorial,<br /> Getting Ready for California Visit,<br /> Astroblast 2007 Presentation<br /> <br /> == Proposal for Radio Observations of T-Tauri Candidates in IC2118 == <br /> <br /> <br /> '''''SUPPORT INFORMATION - T-Tauri Candidates Emit Radio'''''<br /> <br /> '''FROM MATT WALENTOSKY 6/30/2007 @ 2:30 PM - Two Abstracts Below'''<br /> <br /> Title: Radio emission from pre-main-sequence stars<br /> Authors: Skinner, Stephen Lee<br /> <br /> Affiliation: AA(Colorado Univ., Boulder.)<br /> Publication: Ph.D. Thesis Colorado Univ., Boulder.<br /> Publication Date: 01/1992<br /> Category: Space Radiation<br /> Origin: STI<br /> <br /> Abstract<br /> This study focuses on the properties and physical origin of radio continuum emission from pre-main-sequence (PMS) stars. These are young stars, typically less than a few million years old, and are still in a phase of gravitational contraction that will ultimately be halted by the onset of hydrogen burning in their cores. First, I address the question of the origin of centimeter continuum emission in intermediate mass (approx. equal to 3-20 solar mass) PMS stars, the so-called 'Herbig Ae/Be stars'. A high-sensitivity radio survey of 57 such stars was undertaken using the Very Large Array and Australia Telescope, resulting in the detection of twelve stars. These observations provide a homogenous data base consisting of information on source sizes, radio luminosities, variability timescales, circular polarization, and spectral energy distributions in the wavelength range 2-20 cm. Using these data along with previously published spectroscopy, I conclude that centimeter radio emission from Herbig Ae/Be stars is predominantly thermal and in many cases wind-related. An unexpected result of the above program was the serendipitous detection of circularly polarized radio emission in the low mass (approx. equal to 1 solar mass) PMS star Hubble 4, a member of the class of 'weak-lined T Tauri stars' (WTTS). This provides some of the most convincing evidence to date for the existence of ordered magnetic fields in WTTS. In a second observing program, I have searched for evidence of cold (less than or equal to 50 K) circumstellar dust around WTTS, which might exist in the form of remnant disks. Of the sixteen WTTS that were observed in the wavelength range 450-1100 microns using the James Clerk Maxwell Telescope, only V836 Tau was detected. Its spectral energy distribution longward of 10 microns is consistent with that expected for a flat, axisymmetric circumstellar disk of mass approx. equal to 0.04 solar mass (= 42 Jupiter masses). This star may be a rare example of an object in which disk dispersal is underway, but not yet complete.<br /> <br /> <br /> Title: Centimeter Radio Emission from Low-Mass Weak T Tauri Stars in Taurus-Auriga<br /> Authors: Chiang, Eugene; Phillips, R. B.<br /> <br /> Affiliation: AA(MIT), AB(MIT Haystack Observatory)<br /> Publication: American Astronomical Society, 185th AAS Meeting, #48.08; Bulletin of the American Astronomical Society, Vol. 26, p.1388<br /> Publication Date: 12/1994<br /> Origin: AAS<br /> Abstract Copyright:(c) 1994: American Astronomical Society<br /> <br /> Abstract<br /> We report on the results of a sensitive survey for lambda 3.6 cm radio emission from low-mass, weak T Tauri (WTT) stars in the Taurus-Auriga cloud complex. The target population consists of stars in the Herbig and Bell Catalog of spectral type K7 or later, and W(Hα ) &lt;= 10 Angstroms. Of the 28 such stars surveyed using the Very Large Array down to detection thresholds of ~ 0.1 mJy, 7 (possibly 8) are observed to emit at strengths ranging from 0.1 to 2 mJy. Five of these young radio stars are newly discovered in our survey: V827 Tau and V710 Tau B are discovered to be relatively strong sources of mJy emission, while IW Tau, UX Tau B, and the possible detection LkHa 332-G1 form a new population of relatively weak emitters. Our radio survey and complementary surveys are pooled, and of 43 WTT stars K7 or later in Tau-Aur, 14 are now known to be radio emitters at lambda 6 and lambda 3.6 cm. Correlations between radio luminosity and other stellar parameters have been attempted but generally yield null results. Wide binarity (component separations in excess of 0''.13, 20 AU) appears unrelated to radio emission, as does spectral type. Furthermore, we find no convincing evidence for the extreme youth of radio stars, contrary to claims in the literature over the past decade. While we do find that radio-loud stars in our sample are formally younger than the radio-quiet stars by about 0.5 Myr, the reality of this relatively small age difference is highly suspect given uncertainties in the placement of these stars on the HR diagram. Moreover, Monte Carlo-type calculations involving distributing the stars on both the HR diagram and local CO gas density cast doubts on any differences between the radio stars and the general WTT population. We conclude that the age effect for low-mass radio WTT stars in Tau-Aur, if real, is much smaller than previous estimations by factors of 4-10. It is also possible centimeter wavelength surveys to date have still not properly described the radio luminosity function of low-mass WTT stars in Tau-Aur, and we urge future observations of these young stars with denser temporal coverage.<br /> <br /> '''FROM SPUCK 6/30/2007 @ 2:35pm'''<br /> <br /> I'm not sure that we will be able to use the GBT telescope in Green Bank for observations. The beamwidth at 10-15 GHz is probably too big.<br /> <br /> Here are the specs for the GBT<br /> Beamwidth (Table 3) Diffraction beamwidth (FWHM)<br /> 8 GHz it is 90&quot;, <br /> 20 GHz it is 36&quot;, <br /> 50 GHz it is 14&quot;<br /> <br /> Here are some questions from Sue Ann Heatherly at NRAO-Green Bank - One question I have is: is the resolving<br /> power of the GBT sufficient to distinguish spatially between individual stars? Does large scale emission exist within the nebula that will confuse your results?<br /> <br /> The VLA is probably the only instrument that can be used.<br /> <br /> Synthesized Beamwidth (arcsec)depending on configuration<br /> '''Nick Kelley 6/30/2007 3:00PM''' <br /> <br /> 400 cm 24.0&quot; 80.0&quot; 260.0&quot; 850.0&quot;<br /> <br /> 90 cm 6.0&quot; 17.0&quot; 56.0&quot; 200.0&quot; <br /> <br /> 20 cm 1.4 &quot; 3.9&quot; 12.5&quot; 44.0&quot; <br /> <br /> 6 cm 0.4 &quot; 1.2&quot;&quot;&quot; 3.9 &quot; 14.0 &quot;<br /> <br /> 3.6 cm 0.24 &quot; 0.7&quot; 2.3 &quot; 8.4 &quot;<br /> <br /> 2 cm 0.14 &quot; 0.4 &quot; 1.2&quot; 3.9&quot;<br /> <br /> 1.3 cm 0.08 &quot; 0.3&quot; 0.9 &quot;2.8&quot; <br /> <br /> 0.7 cm 0.05 0.15 0.47 1<br /> restricting my creativity<br /> <br /> == T-Tauri/IC2118 Presentation for Astroblast 2007 ==<br /> <br /> '''''Oil City High School students will be presenting August 11 at the Oil Region Astronomical Observatory'''''<br /> <br /> <br /> <br /> FROM Nicholas James Kelley <br /> <br /> Astroblast is amazin ... see pic<br /> <br /> [[Image: astroblast1.JPG|center]]<br /> <br /> == Monitoring T-Tauri Stars using the Perth Obervatory Telescope ==<br /> <br /> '''Generating Light Curves'''<br /> <br /> Using Perth Telescope<br /> <br /> 1. Check to see what the current sky conditions are by checking the live camera<br /> <br /> http://www.perthobservatory.wa.gov.au//information/po_sky_camera.html<br /> <br /> 2. Check to see what the current weather conditions are<br /> <br /> http://www.perthobservatory.wa.gov.au//information/po_weather.html<br /> <br /> 3. Weather forecast for Perth - http://www.bom.gov.au/weather/wa/<br /> <br /> Log into telescope if conditions look good.<br /> <br /> http://perthobservatory.org or http://202.72.190.15<br /> <br /> EMAIL tspuck@hotmail.com for telescope access<br /> <br /> == Chandra X-Ray Data ==<br /> <br /> '''''To date no X-Ray data for IC2118 has been located.''''' If you know of any please contact Tim Spuck at tspuck@hotmail.com.<br /> <br /> == Kitt Peak H-alpha Data ==<br /> <br /> '''''In January of 2007 students from Oil City High School used the 0.9 Meter Telescope at Kitt peak to image regions of IC2118 in H-alpha.''''<br /> <br /> Matt Walentosky, Nick Kelley, Sandy Weiser were the students who went!!!!!!<br /> <br /> == USNO U, B, V, R, and I Data ==<br /> <br /> '''''U, B, V, R, and I data will be used to generate more accurate SEDs for the T-Tauri Candidates'''''<br /> <br /> == Outflows or Jets ==<br /> <br /> '''''Visible outflows or jets are strong evidence that a candidate is indeed a T-Tauri Star'''''<br /> <br /> <br /> <br /> == Multi Wavelength Composite Images ==<br /> <br /> '''''Images and Methods'''''<br /> <br /> FROM SPUCK 6/30/2007 See Image Below- IC 2118 3.6 µm (blue), 5.8 µm (green), 8.0 µm (red) tri-color composite generated using MaxIm DL. (By M. Heath, N. Kelley, P. Morton, M. Walentosky, S. Weiser – Oil City High School, Oil City, PA)<br /> <br /> [[Image: spuckim3.JPG|center]]</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:Main_Page&diff=1851 Talk:Main Page 2007-06-30T19:55:28Z <p>Mattw: /* Proposal for Radio Observations of T-Tauri Candidates in IC2118 */</p> <hr /> <div>== Planning for work session June 29 and/or June 30th for Oil City Students ==<br /> <br /> Matt, Matt, Nick, Greg, Danni, Alexis, and Sandy,<br /> <br /> We had tentatively planned to meet to work on Spitzer stuff and get ready for California on Friday June 29 and/or Saturday June 30. We could meet at the high school something that might be a bit more relaxed is to meet here at my house near Pine City. Please make comments here at the Wiki site as to what your schedule is like and whether or not you can make a work session. Please do this ASAP so we can decide what will work.<br /> <br /> Thanks, Mr. Spuck<br /> <br /> Anytime on Saturday the 30th is good for me. I can not make it on the 29th because my brother is arriving from New Jersey that day. Where exactly in Pine City do you live? Could you send directions to my email? Matt H.<br /> <br /> FROM SPUCK - <br /> - Turn LEFT onto E 1ST ST / US-62 N. Continue to follow US-62 N. Go 2.9 miles Map <br /> <br /> - US-62 N becomes PA-157. Go 13.5 miles Map <br /> <br /> - Turn SLIGHT RIGHT onto PA-208. Go 3.7 miles Map <br /> <br /> - Turn RIGHT onto MILLERSTOWN RD. Go 1.4 miles <br /> <br /> - Gravel lane is on right hand side. Come up lane about 1000 feet.<br /> <br /> [[Image: directions.JPG|center]]<br /> <br /> <br /> <br /> How late into saturday are you planning to work saturday b/c i can't be there until like 1 o'clock earliest!! MATT W.<br /> <br /> FROM SPUCK - Is there another day that works better for everyone ... for example Monday morning July 2 into MOnday afternoon??? Please let me know what your schedule is. Also, keep in mind when you make comments that this discussion page is something that can be viewed by the entire world. This is ok, because we want other teacher/student research teams to see first hand the both the good and bad of trying to conduct student teacher research. We are kind of like the &quot;reality TV show&quot; only on the web. :) Thanks, please respond ASAP. Mr. Spuck<br /> <br /> I am gonna be gone from the July 1st to the 6th in Virginia. I was talking to Nick Kelley and he was saying that he can make it on the 30th anytime like me. Whatever time Matt W. can make the meeting is fine with me and Nick!! Also Greg is currently in Washington DC with a biology seminar and will not be back till July 3rd. He wanted me to fill him in with all the info he is gonna miss when he gets back. Matt H.<br /> <br /> FROM SPUCK - Ok ... it looks like we will meet on Saturday (June 30th). Has anyone spoken to Danni or Alexis?? So where do we want to meet and what time? I'm not sure what condition my room is at the high school because of summer cleaning. I will know more tomorrow when I go up to the school. If we meet at my place, I think we should start BY 10:00 AM and plan on going till about 5:00 PM. If your parents could bring you out, then I could get you back to the Oil City area by 6:00 PM on Saturday, or they can pick you up. Let me know what you think. Matt H. ... have you been in recent contact with Nick? Why has he not posted on the Wiki? Thanks.<br /> <br /> I have been talking to Nick about our upcoming meeting this weekend. However right now Nick is grounded and I believe he can not use the internet.(not sure totally) Also that time at your house is fine with me. Though I might have to be leaving an hour early but right now I'm not certain, I will find out tomorrow and post it up here. Also I will try to get a hold of Nick to tell him about the meeting. Matt H.<br /> <br /> SaturdaY IS THE BEST DAy for me i work 11pm to 7am sundaye night and i work 11pm 7am monday night so that wont work<br /> <br /> FROM SPUCK - I'll assume the comments above are from Nick Kelley. I'f wrong please let me know. I checked my room out yesterday at the high school and everything has been removed for cleaning. So I guess it is my house (see directions above). Plan on arriving between 9:30 and 10:00 AM and we will plan on stopping right around 5:00 PM. Either your parents could pick you up at 5:00 PM or I'll be going to Oil City around 6:00 PM on Saturday and I could give you a ride. If I have this correct it will be Nick at Matt H, with Matt W coming by in the afternoon. Anyone else?<br /> <br /> Sounds right to me... Matt W.<br /> <br /> DANI- account up and running. w00o<br /> <br /> FROM SPUCK - Dani, Matt H, Matt W, and Nick K met and worked on the following:<br /> Using the Perth Telescope,<br /> Radio Proposal,<br /> Wiki Discussion Links,<br /> WZ Sge Observations,<br /> Review of Luisa's Tutorial,<br /> Getting Ready for California Visit,<br /> Astroblast 2007 Presentation<br /> <br /> == Proposal for Radio Observations of T-Tauri Candidates in IC2118 == <br /> <br /> <br /> '''''SUPPORT INFORMATION - T-Tauri Candidates Emit Radio'''''<br /> <br /> '''FROM MATT WALENTOSKY 6/30/2007 @ 2:30 PM - Two Abstracts Below'''<br /> <br /> Title: Radio emission from pre-main-sequence stars<br /> Authors: Skinner, Stephen Lee<br /> <br /> Affiliation: AA(Colorado Univ., Boulder.)<br /> Publication: Ph.D. Thesis Colorado Univ., Boulder.<br /> Publication Date: 01/1992<br /> Category: Space Radiation<br /> Origin: STI<br /> <br /> Abstract<br /> This study focuses on the properties and physical origin of radio continuum emission from pre-main-sequence (PMS) stars. These are young stars, typically less than a few million years old, and are still in a phase of gravitational contraction that will ultimately be halted by the onset of hydrogen burning in their cores. First, I address the question of the origin of centimeter continuum emission in intermediate mass (approx. equal to 3-20 solar mass) PMS stars, the so-called 'Herbig Ae/Be stars'. A high-sensitivity radio survey of 57 such stars was undertaken using the Very Large Array and Australia Telescope, resulting in the detection of twelve stars. These observations provide a homogenous data base consisting of information on source sizes, radio luminosities, variability timescales, circular polarization, and spectral energy distributions in the wavelength range 2-20 cm. Using these data along with previously published spectroscopy, I conclude that centimeter radio emission from Herbig Ae/Be stars is predominantly thermal and in many cases wind-related. An unexpected result of the above program was the serendipitous detection of circularly polarized radio emission in the low mass (approx. equal to 1 solar mass) PMS star Hubble 4, a member of the class of 'weak-lined T Tauri stars' (WTTS). This provides some of the most convincing evidence to date for the existence of ordered magnetic fields in WTTS. In a second observing program, I have searched for evidence of cold (less than or equal to 50 K) circumstellar dust around WTTS, which might exist in the form of remnant disks. Of the sixteen WTTS that were observed in the wavelength range 450-1100 microns using the James Clerk Maxwell Telescope, only V836 Tau was detected. Its spectral energy distribution longward of 10 microns is consistent with that expected for a flat, axisymmetric circumstellar disk of mass approx. equal to 0.04 solar mass (= 42 Jupiter masses). This star may be a rare example of an object in which disk dispersal is underway, but not yet complete.<br /> <br /> <br /> Title: Centimeter Radio Emission from Low-Mass Weak T Tauri Stars in Taurus-Auriga<br /> Authors: Chiang, Eugene; Phillips, R. B.<br /> <br /> Affiliation: AA(MIT), AB(MIT Haystack Observatory)<br /> Publication: American Astronomical Society, 185th AAS Meeting, #48.08; Bulletin of the American Astronomical Society, Vol. 26, p.1388<br /> Publication Date: 12/1994<br /> Origin: AAS<br /> Abstract Copyright:(c) 1994: American Astronomical Society<br /> <br /> Abstract<br /> We report on the results of a sensitive survey for lambda 3.6 cm radio emission from low-mass, weak T Tauri (WTT) stars in the Taurus-Auriga cloud complex. The target population consists of stars in the Herbig and Bell Catalog of spectral type K7 or later, and W(Hα ) &lt;= 10 Angstroms. Of the 28 such stars surveyed using the Very Large Array down to detection thresholds of ~ 0.1 mJy, 7 (possibly 8) are observed to emit at strengths ranging from 0.1 to 2 mJy. Five of these young radio stars are newly discovered in our survey: V827 Tau and V710 Tau B are discovered to be relatively strong sources of mJy emission, while IW Tau, UX Tau B, and the possible detection LkHa 332-G1 form a new population of relatively weak emitters. Our radio survey and complementary surveys are pooled, and of 43 WTT stars K7 or later in Tau-Aur, 14 are now known to be radio emitters at lambda 6 and lambda 3.6 cm. Correlations between radio luminosity and other stellar parameters have been attempted but generally yield null results. Wide binarity (component separations in excess of 0''.13, 20 AU) appears unrelated to radio emission, as does spectral type. Furthermore, we find no convincing evidence for the extreme youth of radio stars, contrary to claims in the literature over the past decade. While we do find that radio-loud stars in our sample are formally younger than the radio-quiet stars by about 0.5 Myr, the reality of this relatively small age difference is highly suspect given uncertainties in the placement of these stars on the HR diagram. Moreover, Monte Carlo-type calculations involving distributing the stars on both the HR diagram and local CO gas density cast doubts on any differences between the radio stars and the general WTT population. We conclude that the age effect for low-mass radio WTT stars in Tau-Aur, if real, is much smaller than previous estimations by factors of 4-10. It is also possible centimeter wavelength surveys to date have still not properly described the radio luminosity function of low-mass WTT stars in Tau-Aur, and we urge future observations of these young stars with denser temporal coverage.<br /> <br /> '''FROM SPUCK 6/30/2007 @ 2:35pm'''<br /> <br /> I'm not sure that we will be able to use the GBT telescope in Green Bank for observations. The beamwidth at 10-15 GHz is probably too big.<br /> <br /> Here are the specs for the GBT<br /> Beamwidth (Table 3) Diffraction beamwidth (FWHM)<br /> 8 GHz it is 90&quot;, <br /> 20 GHz it is 36&quot;, <br /> 50 GHz it is 14&quot;<br /> <br /> Here are some questions from Sue Ann Heatherly at NRAO-Green Bank - One question I have is: is the resolving<br /> power of the GBT sufficient to distinguish spatially between individual stars? Does large scale emission exist within the nebula that will confuse your results?<br /> <br /> The VLA is probably the only instrument that can be used.<br /> <br /> Synthesized Beamwidth (arcsec)depending on configuration<br /> '''Nick Kelley 6/30/2007 3:00PM''' <br /> <br /> 400 cm 24.0&quot; 80.0&quot; 260.0&quot; 850.0&quot;<br /> <br /> 90 cm 6.0&quot; 17.0&quot; 56.0&quot; 200.0&quot; <br /> <br /> 20 cm 1.4 &quot; 3.9&quot; 12.5&quot; 44.0&quot; <br /> <br /> 6 cm 0.4 &quot; 1.2&quot;&quot;&quot; 3.9 &quot; 14.0 &quot;<br /> <br /> 3.6 cm 0.24 &quot; 0.7&quot; 2.3 &quot; 8.4 &quot;<br /> <br /> 2 cm 0.14 &quot; 0.4 &quot; 1.2&quot; 3.9&quot;<br /> <br /> 1.3 cm 0.08 &quot; 0.3&quot; 0.9 &quot;2.8&quot; <br /> <br /> 0.7 cm 0.05 0.15 0.47 1<br /> restricting my creativity<br /> <br /> == T-Tauri/IC2118 Presentation for Astroblast 2007 ==<br /> <br /> '''''Oil City High School students will be presenting August 11 at the Oil Region Astronomical Observatory'''''<br /> <br /> <br /> <br /> FROM Nicholas James Kelley <br /> <br /> Astroblast is amazin ... see pic<br /> <br /> [[Image: astroblast1.JPG|center]]<br /> <br /> == Monitoring T-Tauri Stars using the Perth Obervatory Telescope ==<br /> <br /> '''Generating Light Curves'''<br /> <br /> Using Perth Telescope<br /> <br /> 1. Check to see what the current sky conditions are by checking the live camera<br /> <br /> http://www.perthobservatory.wa.gov.au//information/po_sky_camera.html<br /> <br /> 2. Check to see what the current weather conditions are<br /> <br /> http://www.perthobservatory.wa.gov.au//information/po_weather.html<br /> <br /> 3. Weather forecast for Perth - http://www.bom.gov.au/weather/wa/<br /> <br /> Log into telescope if conditions look good.<br /> <br /> http://perthobservatory.org or http://202.72.190.15<br /> <br /> EMAIL tspuck@hotmail.com for telescope access<br /> <br /> == Chandra X-Ray Data ==<br /> <br /> '''''To date no X-Ray data for IC2118 has been located.''''' If you know of any please contact Tim Spuck at tspuck@hotmail.com.<br /> <br /> == Kitt Peak H-alpha Data ==<br /> <br /> '''''In January of 2007 students from Oil City High School used the 0.9 Meter Telescope at Kitt peak to image regions of IC2118 in H-alpha.''''<br /> <br /> matt was one one of them!!<br /> <br /> == USNO U, B, V, R, and I Data ==<br /> <br /> '''''U, B, V, R, and I data will be used to generate more accurate SEDs for the T-Tauri Candidates'''''<br /> <br /> == Outflows or Jets ==<br /> <br /> '''''Visible outflows or jets are strong evidence that a candidate is indeed a T-Tauri Star'''''<br /> <br /> <br /> <br /> == Multi Wavelength Composite Images ==<br /> <br /> '''''Images and Methods'''''<br /> <br /> FROM SPUCK 6/30/2007 See Image Below- IC 2118 3.6 µm (blue), 5.8 µm (green), 8.0 µm (red) tri-color composite generated using MaxIm DL. (By M. Heath, N. Kelley, P. Morton, M. Walentosky, S. Weiser – Oil City High School, Oil City, PA)<br /> <br /> [[Image: spuckim3.JPG|center]]</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:Main_Page&diff=1830 Talk:Main Page 2007-06-30T19:09:32Z <p>Mattw: /* Kitt Peak H-alpha Data */</p> <hr /> <div>== Planning for work session June 29 and/or June 30th for Oil City Students ==<br /> <br /> Matt, Matt, Nick, Greg, Danni, Alexis, and Sandy,<br /> <br /> We had tentatively planned to meet to work on Spitzer stuff and get ready for California on Friday June 29 and/or Saturday June 30. We could meet at the high school something that might be a bit more relaxed is to meet here at my house near Pine City. Please make comments here at the Wiki site as to what your schedule is like and whether or not you can make a work session. Please do this ASAP so we can decide what will work.<br /> <br /> Thanks, Mr. Spuck<br /> <br /> Anytime on Saturday the 30th is good for me. I can not make it on the 29th because my brother is arriving from New Jersey that day. Where exactly in Pine City do you live? Could you send directions to my email? Matt H.<br /> <br /> FROM SPUCK - <br /> - Turn LEFT onto E 1ST ST / US-62 N. Continue to follow US-62 N. Go 2.9 miles Map <br /> <br /> - US-62 N becomes PA-157. Go 13.5 miles Map <br /> <br /> - Turn SLIGHT RIGHT onto PA-208. Go 3.7 miles Map <br /> <br /> - Turn RIGHT onto MILLERSTOWN RD. Go 1.4 miles <br /> <br /> - Gravel lane is on right hand side. Come up lane about 1000 feet.<br /> <br /> [[Image: directions.JPG|center]]<br /> <br /> <br /> <br /> How late into saturday are you planning to work saturday b/c i can't be there until like 1 o'clock earliest!! MATT W.<br /> <br /> FROM SPUCK - Is there another day that works better for everyone ... for example Monday morning July 2 into MOnday afternoon??? Please let me know what your schedule is. Also, keep in mind when you make comments that this discussion page is something that can be viewed by the entire world. This is ok, because we want other teacher/student research teams to see first hand the both the good and bad of trying to conduct student teacher research. We are kind of like the &quot;reality TV show&quot; only on the web. :) Thanks, please respond ASAP. Mr. Spuck<br /> <br /> I am gonna be gone from the July 1st to the 6th in Virginia. I was talking to Nick Kelley and he was saying that he can make it on the 30th anytime like me. Whatever time Matt W. can make the meeting is fine with me and Nick!! Also Greg is currently in Washington DC with a biology seminar and will not be back till July 3rd. He wanted me to fill him in with all the info he is gonna miss when he gets back. Matt H.<br /> <br /> FROM SPUCK - Ok ... it looks like we will meet on Saturday (June 30th). Has anyone spoken to Danni or Alexis?? So where do we want to meet and what time? I'm not sure what condition my room is at the high school because of summer cleaning. I will know more tomorrow when I go up to the school. If we meet at my place, I think we should start BY 10:00 AM and plan on going till about 5:00 PM. If your parents could bring you out, then I could get you back to the Oil City area by 6:00 PM on Saturday, or they can pick you up. Let me know what you think. Matt H. ... have you been in recent contact with Nick? Why has he not posted on the Wiki? Thanks.<br /> <br /> I have been talking to Nick about our upcoming meeting this weekend. However right now Nick is grounded and I believe he can not use the internet.(not sure totally) Also that time at your house is fine with me. Though I might have to be leaving an hour early but right now I'm not certain, I will find out tomorrow and post it up here. Also I will try to get a hold of Nick to tell him about the meeting. Matt H.<br /> <br /> SaturdaY IS THE BEST DAy for me i work 11pm to 7am sundaye night and i work 11pm 7am monday night so that wont work<br /> <br /> FROM SPUCK - I'll assume the comments above are from Nick Kelley. I'f wrong please let me know. I checked my room out yesterday at the high school and everything has been removed for cleaning. So I guess it is my house (see directions above). Plan on arriving between 9:30 and 10:00 AM and we will plan on stopping right around 5:00 PM. Either your parents could pick you up at 5:00 PM or I'll be going to Oil City around 6:00 PM on Saturday and I could give you a ride. If I have this correct it will be Nick at Matt H, with Matt W coming by in the afternoon. Anyone else?<br /> <br /> Sounds right to me... Matt W.<br /> <br /> DANI- account up and running. w00o<br /> <br /> == Proposal for Radio Observations of T-Tauri Candidates in IC2118 ==<br /> Here is the original proposal we sent in... Matt Walentosky<br /> <br /> Confirmation of T-Tauri Candidates in IC2118<br /> OCHS Research Team<br /> Oil City Sr. High School, Oil City, PA <br /> Teacher: Tim Spuck, 2006<br /> <br /> Tauri Star- a star, with mass from 0.5 to 2.5 solar masses, in an early stage of formation at the which interaction with its associated nebulosity, as well as possible internal instabilities, make it variable in luminosity and render its spectrum very peculiar, also known as nebular variable.<br /> <br /> Introduction<br /> Our research group from Oil City High School in Oil City Pennsylvania is applying for time on the NRAO GBT telescope in Greenbank West Virginia. We plan to use the telescope to image the Witch Head Nebula (IC2118) as part of our ongoing T-Tauri research project. <br /> T-Tauri stars are low mass sun-like stars that are in their early stages of formation, and are found in regions of dense nebulosity. Using the Spitzer Space Telescope’s IRAC and MIPS imagers, members of our student research team (Sandy Weiser and Matt Heath) and our advisor (Tim Spuck) imaged IC 2118 in summer of 2006. During data analysis this past summer, the team identified approximately 200 potential T-Tauri candidates using spectral energy distribution (SEDS) plots and color-color diagrams. However, the SED’s were made using only infrared data. In order to generate more accurate SED’s, and additional color-color diagrams, we must obtain magnitude data for the T-Tauri candidates at radio wavelengths.<br /> Using the GBT we plan to create a mosaic of the region imaged by Spitzer at radio wavelengths. The GBT is necessary because it has sufficient aperture to detect many of the fainter candidates that we otherwise would not be able to detect using smaller radio telescopes, within the National Radio Telescope Observatories.<br /> <br /> We are looking at new stars in the IC2118 region (Witch Head Nebula) in order to complete our portfolio of images from this region. Considering that T-Tauri stars emit radio waves sometimes up to 1000 times more strongly than a mature star (Mendez). We need the visible radio wave images to examine exactly if these new star candidates are T-Tauri stars. It is important for us to use the specific telescope because of its size. This telescope is the only telescope large enough to pick up the faint images of the T-Tauri stars that we have chosen by looking at the data that we have received from Spitzer Science Laboratory in Pasadena California, as well as the Kitt Peak .9 meter and 200 in. spectra telescope in Palomar. This data show that certain stars that we have picked to look at through the radio wave filter is the GBT. Our main goal is to make a mosaic of the IC2118 region from the images that we receive from GBT. Our priority at the observatory is to collect images at a few centimeters. These images are vital to our research team because we need to compare them to the results that we gathered from our previous time looking at the IC2118 region through the Spitzer Space Telescope, Kitt Peak .9 meter, and Palomar 200 inch spectra telescope.<br /> <br /> As to why we are doing this project we are doing this for the same reason that any scientist does research. We are doing this to further understand and comprehend our universe and solar system particularly our sun. Since the time has long since past that we can observe our star from a T-Tauri stage. We must do the next best thing by observing similar stars from the T-Tauri stage.<br /> <br /> Our project consists of:<br /> <br /> T-tauri Star- a star, with mass from 0.5 to 2.5 solar masses, in an early stage of formation at the which interaction with its associated nebulosity, as well as possible internal instabilities, make it variable in luminosity and render its spectrum very peculiar, also known as nebular variable.<br /> <br /> IC2118 is the region of the sky we wish to study b/c of the large presence of T-Tauri stars in the Witch Head Nebula which is part of the IC2118.<br /> <br /> We believe T-Tauri stars are particularly important to study because they resemble our solar system’s star the sun so much. In order for us to completely understand our star, we must understand how it existed in all of its phases. Since the time as our sun’s existence as a T-Tauri star has come and gone we must do the next best thing by studying a observing similar stars.<br /> <br /> The frequency we want to observe the region IC2118 is between two to three centimeters. This is the frequency that we were advised most T-tauri stars emit radio waves at (Dr. Roberto Mendez, Univ. of Hawaii). Using the standard equation Frequency = speed of light/wavelength. We have determined that the best way to observe T-Tauri stars is at 10 GHz and 15GHz.<br /> <br /> We will use IDL to determine radio magnitudes. We will use Microsoft Excel to plot spectral energy distributions (SEDS) and to make color-color diagrams.<br /> <br /> We want to know how many candidate T-tauri stars are actually T-tauri stars. We will be summarizing our findings in a formal research paper to be submitted to the TLRBSE Journal. In addition, members of the group will present their work to the Pennsylvania Government in Harrisburg May 12th -13th; as well as at Astroblast at the Oil Region Astronomical Society. We will also be entering this project into the Pittsburgh Regional Science and Engineering Fair, the Pennsylvania Science Teachers Association Annual Meeting, and hopefully the 2008 American Astronomical Society Conference.<br /> Our team understands that time on your telescope is very prestigious and we will accurately and wisely us any time you would be willing to grant us. As to the time tables, we would prefer, October seems to be a good time to view our candidates, they would be visible from 1 am to 8 am. <br /> <br /> <br /> Nicholas Kelley, Matt Heath, Matt Walentosky, Sandra Weiser, Timothy Spuck <br /> <br /> <br /> '''''SUPPORT INFORMATION - T-Tauri Candidates Emit Radio'''''<br /> <br /> '''FROM MATT WALENTOSKY 6/30/2007 @ 2:30 PM - Two Abstracts Below'''<br /> <br /> Title: Radio emission from pre-main-sequence stars<br /> Authors: Skinner, Stephen Lee<br /> <br /> Affiliation: AA(Colorado Univ., Boulder.)<br /> Publication: Ph.D. Thesis Colorado Univ., Boulder.<br /> Publication Date: 01/1992<br /> Category: Space Radiation<br /> Origin: STI<br /> <br /> Abstract<br /> This study focuses on the properties and physical origin of radio continuum emission from pre-main-sequence (PMS) stars. These are young stars, typically less than a few million years old, and are still in a phase of gravitational contraction that will ultimately be halted by the onset of hydrogen burning in their cores. First, I address the question of the origin of centimeter continuum emission in intermediate mass (approx. equal to 3-20 solar mass) PMS stars, the so-called 'Herbig Ae/Be stars'. A high-sensitivity radio survey of 57 such stars was undertaken using the Very Large Array and Australia Telescope, resulting in the detection of twelve stars. These observations provide a homogenous data base consisting of information on source sizes, radio luminosities, variability timescales, circular polarization, and spectral energy distributions in the wavelength range 2-20 cm. Using these data along with previously published spectroscopy, I conclude that centimeter radio emission from Herbig Ae/Be stars is predominantly thermal and in many cases wind-related. An unexpected result of the above program was the serendipitous detection of circularly polarized radio emission in the low mass (approx. equal to 1 solar mass) PMS star Hubble 4, a member of the class of 'weak-lined T Tauri stars' (WTTS). This provides some of the most convincing evidence to date for the existence of ordered magnetic fields in WTTS. In a second observing program, I have searched for evidence of cold (less than or equal to 50 K) circumstellar dust around WTTS, which might exist in the form of remnant disks. Of the sixteen WTTS that were observed in the wavelength range 450-1100 microns using the James Clerk Maxwell Telescope, only V836 Tau was detected. Its spectral energy distribution longward of 10 microns is consistent with that expected for a flat, axisymmetric circumstellar disk of mass approx. equal to 0.04 solar mass (= 42 Jupiter masses). This star may be a rare example of an object in which disk dispersal is underway, but not yet complete.<br /> <br /> <br /> Title: Centimeter Radio Emission from Low-Mass Weak T Tauri Stars in Taurus-Auriga<br /> Authors: Chiang, Eugene; Phillips, R. B.<br /> <br /> Affiliation: AA(MIT), AB(MIT Haystack Observatory)<br /> Publication: American Astronomical Society, 185th AAS Meeting, #48.08; Bulletin of the American Astronomical Society, Vol. 26, p.1388<br /> Publication Date: 12/1994<br /> Origin: AAS<br /> Abstract Copyright:(c) 1994: American Astronomical Society<br /> <br /> Abstract<br /> We report on the results of a sensitive survey for lambda 3.6 cm radio emission from low-mass, weak T Tauri (WTT) stars in the Taurus-Auriga cloud complex. The target population consists of stars in the Herbig and Bell Catalog of spectral type K7 or later, and W(Hα ) &lt;= 10 Angstroms. Of the 28 such stars surveyed using the Very Large Array down to detection thresholds of ~ 0.1 mJy, 7 (possibly 8) are observed to emit at strengths ranging from 0.1 to 2 mJy. Five of these young radio stars are newly discovered in our survey: V827 Tau and V710 Tau B are discovered to be relatively strong sources of mJy emission, while IW Tau, UX Tau B, and the possible detection LkHa 332-G1 form a new population of relatively weak emitters. Our radio survey and complementary surveys are pooled, and of 43 WTT stars K7 or later in Tau-Aur, 14 are now known to be radio emitters at lambda 6 and lambda 3.6 cm. Correlations between radio luminosity and other stellar parameters have been attempted but generally yield null results. Wide binarity (component separations in excess of 0''.13, 20 AU) appears unrelated to radio emission, as does spectral type. Furthermore, we find no convincing evidence for the extreme youth of radio stars, contrary to claims in the literature over the past decade. While we do find that radio-loud stars in our sample are formally younger than the radio-quiet stars by about 0.5 Myr, the reality of this relatively small age difference is highly suspect given uncertainties in the placement of these stars on the HR diagram. Moreover, Monte Carlo-type calculations involving distributing the stars on both the HR diagram and local CO gas density cast doubts on any differences between the radio stars and the general WTT population. We conclude that the age effect for low-mass radio WTT stars in Tau-Aur, if real, is much smaller than previous estimations by factors of 4-10. It is also possible centimeter wavelength surveys to date have still not properly described the radio luminosity function of low-mass WTT stars in Tau-Aur, and we urge future observations of these young stars with denser temporal coverage.<br /> <br /> '''FROM SPUCK 6/30/2007 @ 2:35pm'''<br /> <br /> I'm not sure that we will be able to use the GBT telescope in Green Bank for observations. The beamwidth at 10-15 GHz is probably too big.<br /> <br /> Here are the specs for the GBT<br /> Beamwidth (Table 3) Diffraction beamwidth (FWHM)<br /> 8 GHz it is 90&quot;, <br /> 20 GHz it is 36&quot;, <br /> 50 GHz it is 14&quot;<br /> <br /> Here are some questions from Sue Ann Heatherly at NRAO-Green Bank - One question I have is: is the resolving<br /> power of the GBT sufficient to distinguish spatially between individual stars? Does large scale emission exist within the nebula that will confuse your results?<br /> <br /> The VLA is probably the only instrument that can be used.<br /> <br /> Synthesized Beamwidth (arcsec)depending on configuration<br /> '''Nick Kelley 6/30/2007 3:00PM''' <br /> <br /> 400 cm 24.0&quot; 80.0&quot; 260.0&quot; 850.0&quot;<br /> <br /> 90 cm 6.0&quot; 17.0&quot; 56.0&quot; 200.0&quot; <br /> <br /> 20 cm 1.4 &quot; 3.9&quot; 12.5&quot; 44.0&quot; <br /> <br /> 6 cm 0.4 &quot; 1.2&quot;&quot;&quot; 3.9 &quot; 14.0 &quot;<br /> <br /> 3.6 cm 0.24 &quot; 0.7&quot; 2.3 &quot; 8.4 &quot;<br /> <br /> 2 cm 0.14 &quot; 0.4 &quot; 1.2&quot; 3.9&quot;<br /> <br /> 1.3 cm 0.08 &quot; 0.3&quot; 0.9 &quot;2.8&quot; <br /> <br /> 0.7 cm 0.05 0.15 0.47 1<br /> restricting my creativity<br /> <br /> == T-Tauri/IC2118 Presentation for Astroblast 2007 ==<br /> <br /> '''''Oil City High School students will be presenting August 11 at the Oil Region Astronomical Observatory'''''<br /> <br /> == Monitoring T-Tauri Stars using the Perth Obervatory Telescope ==<br /> <br /> '''Generating Light Curves'''<br /> <br /> Using Perth Telescope<br /> <br /> 1. Check to see what the current sky conditions are by checking the live camera<br /> <br /> http://www.perthobservatory.wa.gov.au//information/po_sky_camera.html<br /> <br /> 2. Check to see what the current weather conditions are<br /> <br /> http://www.perthobservatory.wa.gov.au//information/po_weather.html<br /> <br /> 3. Weather forecast for Perth - http://www.bom.gov.au/weather/wa/<br /> <br /> Log into telescope if conditions look good.<br /> <br /> http://perthobservatory.org or http://202.72.190.15<br /> <br /> EMAIL tspuck@hotmail.com for telescope access<br /> <br /> == Chandra X-Ray Data ==<br /> <br /> '''''To date no X-Ray data for IC2118 has been located.''''' If you know of any please contact Tim Spuck at tspuck@hotmail.com.<br /> <br /> == Kitt Peak H-alpha Data ==<br /> <br /> '''''In January of 2007 students from Oil City High School used the 0.9 Meter Telescope at Kitt peak to image regions of IC2118 in H-alpha.''''<br /> <br /> matt was one one of them!!<br /> <br /> == USNO Data ==<br /> <br /> Edit<br /> <br /> == Out Flows ==<br /> <br /> View in Optical &amp; in IRAC<br /> <br /> == Measuring Brightness ==<br /> <br /> Edit</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:Main_Page&diff=1823 Talk:Main Page 2007-06-30T19:02:49Z <p>Mattw: /* Proposal for Radio Observations of T-Tauri Candidates in IC2118 */</p> <hr /> <div>== Planning for work session June 29 and/or June 30th for Oil City Students ==<br /> <br /> Matt, Matt, Nick, Greg, Danni, Alexis, and Sandy,<br /> <br /> We had tentatively planned to meet to work on Spitzer stuff and get ready for California on Friday June 29 and/or Saturday June 30. We could meet at the high school something that might be a bit more relaxed is to meet here at my house near Pine City. Please make comments here at the Wiki site as to what your schedule is like and whether or not you can make a work session. Please do this ASAP so we can decide what will work.<br /> <br /> Thanks, Mr. Spuck<br /> <br /> Anytime on Saturday the 30th is good for me. I can not make it on the 29th because my brother is arriving from New Jersey that day. Where exactly in Pine City do you live? Could you send directions to my email? Matt H.<br /> <br /> FROM SPUCK - <br /> - Turn LEFT onto E 1ST ST / US-62 N. Continue to follow US-62 N. Go 2.9 miles Map <br /> <br /> - US-62 N becomes PA-157. Go 13.5 miles Map <br /> <br /> - Turn SLIGHT RIGHT onto PA-208. Go 3.7 miles Map <br /> <br /> - Turn RIGHT onto MILLERSTOWN RD. Go 1.4 miles <br /> <br /> - Gravel lane is on right hand side. Come up lane about 1000 feet.<br /> <br /> [[Image: directions.JPG|center]]<br /> <br /> <br /> <br /> How late into saturday are you planning to work saturday b/c i can't be there until like 1 o'clock earliest!! MATT W.<br /> <br /> FROM SPUCK - Is there another day that works better for everyone ... for example Monday morning July 2 into MOnday afternoon??? Please let me know what your schedule is. Also, keep in mind when you make comments that this discussion page is something that can be viewed by the entire world. This is ok, because we want other teacher/student research teams to see first hand the both the good and bad of trying to conduct student teacher research. We are kind of like the &quot;reality TV show&quot; only on the web. :) Thanks, please respond ASAP. Mr. Spuck<br /> <br /> I am gonna be gone from the July 1st to the 6th in Virginia. I was talking to Nick Kelley and he was saying that he can make it on the 30th anytime like me. Whatever time Matt W. can make the meeting is fine with me and Nick!! Also Greg is currently in Washington DC with a biology seminar and will not be back till July 3rd. He wanted me to fill him in with all the info he is gonna miss when he gets back. Matt H.<br /> <br /> FROM SPUCK - Ok ... it looks like we will meet on Saturday (June 30th). Has anyone spoken to Danni or Alexis?? So where do we want to meet and what time? I'm not sure what condition my room is at the high school because of summer cleaning. I will know more tomorrow when I go up to the school. If we meet at my place, I think we should start BY 10:00 AM and plan on going till about 5:00 PM. If your parents could bring you out, then I could get you back to the Oil City area by 6:00 PM on Saturday, or they can pick you up. Let me know what you think. Matt H. ... have you been in recent contact with Nick? Why has he not posted on the Wiki? Thanks.<br /> <br /> I have been talking to Nick about our upcoming meeting this weekend. However right now Nick is grounded and I believe he can not use the internet.(not sure totally) Also that time at your house is fine with me. Though I might have to be leaving an hour early but right now I'm not certain, I will find out tomorrow and post it up here. Also I will try to get a hold of Nick to tell him about the meeting. Matt H.<br /> <br /> SaturdaY IS THE BEST DAy for me i work 11pm to 7am sundaye night and i work 11pm 7am monday night so that wont work<br /> <br /> FROM SPUCK - I'll assume the comments above are from Nick Kelley. I'f wrong please let me know. I checked my room out yesterday at the high school and everything has been removed for cleaning. So I guess it is my house (see directions above). Plan on arriving between 9:30 and 10:00 AM and we will plan on stopping right around 5:00 PM. Either your parents could pick you up at 5:00 PM or I'll be going to Oil City around 6:00 PM on Saturday and I could give you a ride. If I have this correct it will be Nick at Matt H, with Matt W coming by in the afternoon. Anyone else?<br /> <br /> Sounds right to me... Matt W.<br /> <br /> DANI- account up and running. w00o<br /> <br /> == Proposal for Radio Observations of T-Tauri Candidates in IC2118 ==<br /> Here is the original proposal we sent in... Matt Walentosky<br /> <br /> Confirmation of T-Tauri Candidates in IC2118<br /> OCHS Research Team<br /> Oil City Sr. High School, Oil City, PA <br /> Teacher: Tim Spuck, 2006<br /> <br /> Tauri Star- a star, with mass from 0.5 to 2.5 solar masses, in an early stage of formation at the which interaction with its associated nebulosity, as well as possible internal instabilities, make it variable in luminosity and render its spectrum very peculiar, also known as nebular variable.<br /> <br /> Introduction<br /> Our research group from Oil City High School in Oil City Pennsylvania is applying for time on the NRAO GBT telescope in Greenbank West Virginia. We plan to use the telescope to image the Witch Head Nebula (IC2118) as part of our ongoing T-Tauri research project. <br /> T-Tauri stars are low mass sun-like stars that are in their early stages of formation, and are found in regions of dense nebulosity. Using the Spitzer Space Telescope’s IRAC and MIPS imagers, members of our student research team (Sandy Weiser and Matt Heath) and our advisor (Tim Spuck) imaged IC 2118 in summer of 2006. During data analysis this past summer, the team identified approximately 200 potential T-Tauri candidates using spectral energy distribution (SEDS) plots and color-color diagrams. However, the SED’s were made using only infrared data. In order to generate more accurate SED’s, and additional color-color diagrams, we must obtain magnitude data for the T-Tauri candidates at radio wavelengths.<br /> Using the GBT we plan to create a mosaic of the region imaged by Spitzer at radio wavelengths. The GBT is necessary because it has sufficient aperture to detect many of the fainter candidates that we otherwise would not be able to detect using smaller radio telescopes, within the National Radio Telescope Observatories.<br /> <br /> We are looking at new stars in the IC2118 region (Witch Head Nebula) in order to complete our portfolio of images from this region. Considering that T-Tauri stars emit radio waves sometimes up to 1000 times more strongly than a mature star (Mendez). We need the visible radio wave images to examine exactly if these new star candidates are T-Tauri stars. It is important for us to use the specific telescope because of its size. This telescope is the only telescope large enough to pick up the faint images of the T-Tauri stars that we have chosen by looking at the data that we have received from Spitzer Science Laboratory in Pasadena California, as well as the Kitt Peak .9 meter and 200 in. spectra telescope in Palomar. This data show that certain stars that we have picked to look at through the radio wave filter is the GBT. Our main goal is to make a mosaic of the IC2118 region from the images that we receive from GBT. Our priority at the observatory is to collect images at a few centimeters. These images are vital to our research team because we need to compare them to the results that we gathered from our previous time looking at the IC2118 region through the Spitzer Space Telescope, Kitt Peak .9 meter, and Palomar 200 inch spectra telescope.<br /> <br /> As to why we are doing this project we are doing this for the same reason that any scientist does research. We are doing this to further understand and comprehend our universe and solar system particularly our sun. Since the time has long since past that we can observe our star from a T-Tauri stage. We must do the next best thing by observing similar stars from the T-Tauri stage.<br /> <br /> Our project consists of:<br /> <br /> T-tauri Star- a star, with mass from 0.5 to 2.5 solar masses, in an early stage of formation at the which interaction with its associated nebulosity, as well as possible internal instabilities, make it variable in luminosity and render its spectrum very peculiar, also known as nebular variable.<br /> <br /> IC2118 is the region of the sky we wish to study b/c of the large presence of T-Tauri stars in the Witch Head Nebula which is part of the IC2118.<br /> <br /> We believe T-Tauri stars are particularly important to study because they resemble our solar system’s star the sun so much. In order for us to completely understand our star, we must understand how it existed in all of its phases. Since the time as our sun’s existence as a T-Tauri star has come and gone we must do the next best thing by studying a observing similar stars.<br /> <br /> The frequency we want to observe the region IC2118 is between two to three centimeters. This is the frequency that we were advised most T-tauri stars emit radio waves at (Dr. Roberto Mendez, Univ. of Hawaii). Using the standard equation Frequency = speed of light/wavelength. We have determined that the best way to observe T-Tauri stars is at 10 GHz and 15GHz.<br /> <br /> We will use IDL to determine radio magnitudes. We will use Microsoft Excel to plot spectral energy distributions (SEDS) and to make color-color diagrams.<br /> <br /> We want to know how many candidate T-tauri stars are actually T-tauri stars. We will be summarizing our findings in a formal research paper to be submitted to the TLRBSE Journal. In addition, members of the group will present their work to the Pennsylvania Government in Harrisburg May 12th -13th; as well as at Astroblast at the Oil Region Astronomical Society. We will also be entering this project into the Pittsburgh Regional Science and Engineering Fair, the Pennsylvania Science Teachers Association Annual Meeting, and hopefully the 2008 American Astronomical Society Conference.<br /> Our team understands that time on your telescope is very prestigious and we will accurately and wisely us any time you would be willing to grant us. As to the time tables, we would prefer, October seems to be a good time to view our candidates, they would be visible from 1 am to 8 am. <br /> <br /> <br /> Nicholas Kelley, Matt Heath, Matt Walentosky, Sandra Weiser, Timothy Spuck <br /> <br /> <br /> '''''SUPPORT INFORMATION - T-Tauri Candidates Emit Radio'''''<br /> <br /> '''FROM MATT WALENTOSKY 6/30/2007 @ 2:30 PM - Two Abstracts Below'''<br /> <br /> Title: Radio emission from pre-main-sequence stars<br /> Authors: Skinner, Stephen Lee<br /> <br /> Affiliation: AA(Colorado Univ., Boulder.)<br /> Publication: Ph.D. Thesis Colorado Univ., Boulder.<br /> Publication Date: 01/1992<br /> Category: Space Radiation<br /> Origin: STI<br /> <br /> Abstract<br /> This study focuses on the properties and physical origin of radio continuum emission from pre-main-sequence (PMS) stars. These are young stars, typically less than a few million years old, and are still in a phase of gravitational contraction that will ultimately be halted by the onset of hydrogen burning in their cores. First, I address the question of the origin of centimeter continuum emission in intermediate mass (approx. equal to 3-20 solar mass) PMS stars, the so-called 'Herbig Ae/Be stars'. A high-sensitivity radio survey of 57 such stars was undertaken using the Very Large Array and Australia Telescope, resulting in the detection of twelve stars. These observations provide a homogenous data base consisting of information on source sizes, radio luminosities, variability timescales, circular polarization, and spectral energy distributions in the wavelength range 2-20 cm. Using these data along with previously published spectroscopy, I conclude that centimeter radio emission from Herbig Ae/Be stars is predominantly thermal and in many cases wind-related. An unexpected result of the above program was the serendipitous detection of circularly polarized radio emission in the low mass (approx. equal to 1 solar mass) PMS star Hubble 4, a member of the class of 'weak-lined T Tauri stars' (WTTS). This provides some of the most convincing evidence to date for the existence of ordered magnetic fields in WTTS. In a second observing program, I have searched for evidence of cold (less than or equal to 50 K) circumstellar dust around WTTS, which might exist in the form of remnant disks. Of the sixteen WTTS that were observed in the wavelength range 450-1100 microns using the James Clerk Maxwell Telescope, only V836 Tau was detected. Its spectral energy distribution longward of 10 microns is consistent with that expected for a flat, axisymmetric circumstellar disk of mass approx. equal to 0.04 solar mass (= 42 Jupiter masses). This star may be a rare example of an object in which disk dispersal is underway, but not yet complete.<br /> <br /> <br /> Title: Centimeter Radio Emission from Low-Mass Weak T Tauri Stars in Taurus-Auriga<br /> Authors: Chiang, Eugene; Phillips, R. B.<br /> <br /> Affiliation: AA(MIT), AB(MIT Haystack Observatory)<br /> Publication: American Astronomical Society, 185th AAS Meeting, #48.08; Bulletin of the American Astronomical Society, Vol. 26, p.1388<br /> Publication Date: 12/1994<br /> Origin: AAS<br /> Abstract Copyright:(c) 1994: American Astronomical Society<br /> <br /> Abstract<br /> We report on the results of a sensitive survey for lambda 3.6 cm radio emission from low-mass, weak T Tauri (WTT) stars in the Taurus-Auriga cloud complex. The target population consists of stars in the Herbig and Bell Catalog of spectral type K7 or later, and W(Hα ) &lt;= 10 Angstroms. Of the 28 such stars surveyed using the Very Large Array down to detection thresholds of ~ 0.1 mJy, 7 (possibly 8) are observed to emit at strengths ranging from 0.1 to 2 mJy. Five of these young radio stars are newly discovered in our survey: V827 Tau and V710 Tau B are discovered to be relatively strong sources of mJy emission, while IW Tau, UX Tau B, and the possible detection LkHa 332-G1 form a new population of relatively weak emitters. Our radio survey and complementary surveys are pooled, and of 43 WTT stars K7 or later in Tau-Aur, 14 are now known to be radio emitters at lambda 6 and lambda 3.6 cm. Correlations between radio luminosity and other stellar parameters have been attempted but generally yield null results. Wide binarity (component separations in excess of 0''.13, 20 AU) appears unrelated to radio emission, as does spectral type. Furthermore, we find no convincing evidence for the extreme youth of radio stars, contrary to claims in the literature over the past decade. While we do find that radio-loud stars in our sample are formally younger than the radio-quiet stars by about 0.5 Myr, the reality of this relatively small age difference is highly suspect given uncertainties in the placement of these stars on the HR diagram. Moreover, Monte Carlo-type calculations involving distributing the stars on both the HR diagram and local CO gas density cast doubts on any differences between the radio stars and the general WTT population. We conclude that the age effect for low-mass radio WTT stars in Tau-Aur, if real, is much smaller than previous estimations by factors of 4-10. It is also possible centimeter wavelength surveys to date have still not properly described the radio luminosity function of low-mass WTT stars in Tau-Aur, and we urge future observations of these young stars with denser temporal coverage.<br /> <br /> '''FROM SPUCK 6/30/2007 @ 2:35pm'''<br /> <br /> I'm not sure that we will be able to use the GBT telescope in Green Bank for observations. The beamwidth at 10-15 GHz is probably too big.<br /> <br /> Here are the specs for the GBT<br /> Beamwidth (Table 3) Diffraction beamwidth (FWHM)<br /> 8 GHz it is 90&quot;, <br /> 20 GHz it is 36&quot;, <br /> 50 GHz it is 14&quot;<br /> <br /> Here are some questions from Sue Ann Heatherly at NRAO-Green Bank - One question I have is: is the resolving<br /> power of the GBT sufficient to distinguish spatially between individual stars? Does large scale emission exist within the nebula that will confuse your results?<br /> <br /> The VLA is probably the only instrument that can be used.<br /> <br /> Synthesized Beamwidth (arcsec)depending on configuration<br /> '''Nick Kelley 6/30/2007 3:00PM''' <br /> <br /> 400 cm 24.0&quot; 80.0&quot; 260.0&quot; 850.0&quot;<br /> <br /> 90 cm 6.0&quot; 17.0&quot; 56.0&quot; 200.0&quot; <br /> <br /> 20 cm 1.4 &quot; 3.9&quot; 12.5&quot; 44.0&quot; <br /> <br /> 6 cm 0.4 &quot; 1.2&quot;&quot;&quot; 3.9 &quot; 14.0 &quot;<br /> <br /> 3.6 cm 0.24 &quot; 0.7&quot; 2.3 &quot; 8.4 &quot;<br /> <br /> 2 cm 0.14 &quot; 0.4 &quot; 1.2&quot; 3.9&quot;<br /> <br /> 1.3 cm 0.08 &quot; 0.3&quot; 0.9 &quot;2.8&quot; <br /> <br /> 0.7 cm 0.05 0.15 0.47 1<br /> restricting my creativity<br /> <br /> == T-Tauri/IC2118 Presentation for Astroblast 2007 ==<br /> <br /> Oil City High School students will be presenting August 11 at the Oil Region Astronomical Observatory<br /> <br /> == Monitoring T-Tauri Stars using the Perth Obervatory Telescope ==<br /> <br /> Generating light curves<br /> <br /> == Chandra X-Ray Data ==<br /> <br /> No information for IC2118 available to date.<br /> <br /> == Kitt Peak Data ==<br /> <br /> H alpha Data<br /> <br /> == USNO Data ==<br /> <br /> Edit<br /> <br /> == Out Flows ==<br /> <br /> View in Optical &amp; in IRAC</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:Main_Page&diff=1804 Talk:Main Page 2007-06-30T18:30:04Z <p>Mattw: /* Proposal for Radio Observations of T-Tauri Candidates in IC2118 */</p> <hr /> <div>hey this is nick Kelley from Oil City it is going to be fun working with everybody<br /> <br /> == Hello ==<br /> <br /> Hey guys this is Matt Heath from Oil City. I can not wait to work with all of you guys through this wiki.<br /> <br /> sweet<br /> <br /> ITS matt walentosky, does this work?<br /> <br /> == Planning for work session June 29 and/or June 30th for Oil City Students ==<br /> <br /> Matt, Matt, Nick, Greg, Danni, Alexis, and Sandy,<br /> <br /> We had tentatively planned to meet to work on Spitzer stuff and get ready for California on Friday June 29 and/or Saturday June 30. We could meet at the high school something that might be a bit more relaxed is to meet here at my house near Pine City. Please make comments here at the Wiki site as to what your schedule is like and whether or not you can make a work session. Please do this ASAP so we can decide what will work.<br /> <br /> Thanks, Mr. Spuck<br /> <br /> Anytime on Saturday the 30th is good for me. I can not make it on the 29th because my brother is arriving from New Jersey that day. Where exactly in Pine City do you live? Could you send directions to my email? Matt H.<br /> <br /> FROM SPUCK - <br /> - Turn LEFT onto E 1ST ST / US-62 N. Continue to follow US-62 N. Go 2.9 miles Map <br /> <br /> - US-62 N becomes PA-157. Go 13.5 miles Map <br /> <br /> - Turn SLIGHT RIGHT onto PA-208. Go 3.7 miles Map <br /> <br /> - Turn RIGHT onto MILLERSTOWN RD. Go 1.4 miles <br /> <br /> - Gravel lane is on right hand side. Come up lane about 1000 feet.<br /> <br /> [[Image: directions.JPG|center]]<br /> <br /> <br /> <br /> How late into saturday are you planning to work saturday b/c i can't be there until like 1 o'clock earliest!! MATT W.<br /> <br /> FROM SPUCK - Is there another day that works better for everyone ... for example Monday morning July 2 into MOnday afternoon??? Please let me know what your schedule is. Also, keep in mind when you make comments that this discussion page is something that can be viewed by the entire world. This is ok, because we want other teacher/student research teams to see first hand the both the good and bad of trying to conduct student teacher research. We are kind of like the &quot;reality TV show&quot; only on the web. :) Thanks, please respond ASAP. Mr. Spuck<br /> <br /> I am gonna be gone from the July 1st to the 6th in Virginia. I was talking to Nick Kelley and he was saying that he can make it on the 30th anytime like me. Whatever time Matt W. can make the meeting is fine with me and Nick!! Also Greg is currently in Washington DC with a biology seminar and will not be back till July 3rd. He wanted me to fill him in with all the info he is gonna miss when he gets back. Matt H.<br /> <br /> FROM SPUCK - Ok ... it looks like we will meet on Saturday (June 30th). Has anyone spoken to Danni or Alexis?? So where do we want to meet and what time? I'm not sure what condition my room is at the high school because of summer cleaning. I will know more tomorrow when I go up to the school. If we meet at my place, I think we should start BY 10:00 AM and plan on going till about 5:00 PM. If your parents could bring you out, then I could get you back to the Oil City area by 6:00 PM on Saturday, or they can pick you up. Let me know what you think. Matt H. ... have you been in recent contact with Nick? Why has he not posted on the Wiki? Thanks.<br /> <br /> I have been talking to Nick about our upcoming meeting this weekend. However right now Nick is grounded and I believe he can not use the internet.(not sure totally) Also that time at your house is fine with me. Though I might have to be leaving an hour early but right now I'm not certain, I will find out tomorrow and post it up here. Also I will try to get a hold of Nick to tell him about the meeting. Matt H.<br /> <br /> SaturdaY IS THE BEST DAy for me i work 11pm to 7am sundaye night and i work 11pm 7am monday night so that wont work<br /> <br /> FROM SPUCK - I'll assume the comments above are from Nick Kelley. I'f wrong please let me know. I checked my room out yesterday at the high school and everything has been removed for cleaning. So I guess it is my house (see directions above). Plan on arriving between 9:30 and 10:00 AM and we will plan on stopping right around 5:00 PM. Either your parents could pick you up at 5:00 PM or I'll be going to Oil City around 6:00 PM on Saturday and I could give you a ride. If I have this correct it will be Nick at Matt H, with Matt W coming by in the afternoon. Anyone else?<br /> <br /> Sounds right to me... Matt W.<br /> <br /> DANI- account up and running. w00o<br /> <br /> == Proposal for Radio Observations of T-Tauri Candidates in IC2118 ==<br /> <br /> SUPPORT INFORMATION - T-Tauri Candidates Emit Radio<br /> <br /> FROM MATT WALENTOSKY - Two Abstracts Below<br /> <br /> Title: Radio emission from pre-main-sequence stars<br /> Authors: Skinner, Stephen Lee<br /> <br /> Affiliation: AA(Colorado Univ., Boulder.)<br /> Publication: Ph.D. Thesis Colorado Univ., Boulder.<br /> Publication Date: 01/1992<br /> Category: Space Radiation<br /> Origin: STI<br /> <br /> Abstract<br /> This study focuses on the properties and physical origin of radio continuum emission from pre-main-sequence (PMS) stars. These are young stars, typically less than a few million years old, and are still in a phase of gravitational contraction that will ultimately be halted by the onset of hydrogen burning in their cores. First, I address the question of the origin of centimeter continuum emission in intermediate mass (approx. equal to 3-20 solar mass) PMS stars, the so-called 'Herbig Ae/Be stars'. A high-sensitivity radio survey of 57 such stars was undertaken using the Very Large Array and Australia Telescope, resulting in the detection of twelve stars. These observations provide a homogenous data base consisting of information on source sizes, radio luminosities, variability timescales, circular polarization, and spectral energy distributions in the wavelength range 2-20 cm. Using these data along with previously published spectroscopy, I conclude that centimeter radio emission from Herbig Ae/Be stars is predominantly thermal and in many cases wind-related. An unexpected result of the above program was the serendipitous detection of circularly polarized radio emission in the low mass (approx. equal to 1 solar mass) PMS star Hubble 4, a member of the class of 'weak-lined T Tauri stars' (WTTS). This provides some of the most convincing evidence to date for the existence of ordered magnetic fields in WTTS. In a second observing program, I have searched for evidence of cold (less than or equal to 50 K) circumstellar dust around WTTS, which might exist in the form of remnant disks. Of the sixteen WTTS that were observed in the wavelength range 450-1100 microns using the James Clerk Maxwell Telescope, only V836 Tau was detected. Its spectral energy distribution longward of 10 microns is consistent with that expected for a flat, axisymmetric circumstellar disk of mass approx. equal to 0.04 solar mass (= 42 Jupiter masses). This star may be a rare example of an object in which disk dispersal is underway, but not yet complete.<br /> <br /> <br /> Title: Centimeter Radio Emission from Low-Mass Weak T Tauri Stars in Taurus-Auriga<br /> Authors: Chiang, Eugene; Phillips, R. B.<br /> <br /> Affiliation: AA(MIT), AB(MIT Haystack Observatory)<br /> Publication: American Astronomical Society, 185th AAS Meeting, #48.08; Bulletin of the American Astronomical Society, Vol. 26, p.1388<br /> Publication Date: 12/1994<br /> Origin: AAS<br /> Abstract Copyright:(c) 1994: American Astronomical Society<br /> <br /> Abstract<br /> We report on the results of a sensitive survey for lambda 3.6 cm radio emission from low-mass, weak T Tauri (WTT) stars in the Taurus-Auriga cloud complex. The target population consists of stars in the Herbig and Bell Catalog of spectral type K7 or later, and W(Hα ) &lt;= 10 Angstroms. Of the 28 such stars surveyed using the Very Large Array down to detection thresholds of ~ 0.1 mJy, 7 (possibly 8) are observed to emit at strengths ranging from 0.1 to 2 mJy. Five of these young radio stars are newly discovered in our survey: V827 Tau and V710 Tau B are discovered to be relatively strong sources of mJy emission, while IW Tau, UX Tau B, and the possible detection LkHa 332-G1 form a new population of relatively weak emitters. Our radio survey and complementary surveys are pooled, and of 43 WTT stars K7 or later in Tau-Aur, 14 are now known to be radio emitters at lambda 6 and lambda 3.6 cm. Correlations between radio luminosity and other stellar parameters have been attempted but generally yield null results. Wide binarity (component separations in excess of 0''.13, 20 AU) appears unrelated to radio emission, as does spectral type. Furthermore, we find no convincing evidence for the extreme youth of radio stars, contrary to claims in the literature over the past decade. While we do find that radio-loud stars in our sample are formally younger than the radio-quiet stars by about 0.5 Myr, the reality of this relatively small age difference is highly suspect given uncertainties in the placement of these stars on the HR diagram. Moreover, Monte Carlo-type calculations involving distributing the stars on both the HR diagram and local CO gas density cast doubts on any differences between the radio stars and the general WTT population. We conclude that the age effect for low-mass radio WTT stars in Tau-Aur, if real, is much smaller than previous estimations by factors of 4-10. It is also possible centimeter wavelength surveys to date have still not properly described the radio luminosity function of low-mass WTT stars in Tau-Aur, and we urge future observations of these young stars with denser temporal coverage.</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:Main_Page&diff=1797 Talk:Main Page 2007-06-29T17:11:18Z <p>Mattw: </p> <hr /> <div>hey this is nick Kelley from Oil City it is going to be fun working with everybody<br /> <br /> == Hello ==<br /> <br /> Hey guys this is Matt Heath from Oil City. I can not wait to work with all of you guys through this wiki.<br /> <br /> sweet<br /> <br /> ITS matt walentosky, does this work?<br /> <br /> == Planning for work session June 29 and/or June 30th for Oil City Students ==<br /> <br /> Matt, Matt, Nick, Greg, Danni, Alexis, and Sandy,<br /> <br /> We had tentatively planned to meet to work on Spitzer stuff and get ready for California on Friday June 29 and/or Saturday June 30. We could meet at the high school something that might be a bit more relaxed is to meet here at my house near Pine City. Please make comments here at the Wiki site as to what your schedule is like and whether or not you can make a work session. Please do this ASAP so we can decide what will work.<br /> <br /> Thanks, Mr. Spuck<br /> <br /> Anytime on Saturday the 30th is good for me. I can not make it on the 29th because my brother is arriving from New Jersey that day. Where exactly in Pine City do you live? Could you send directions to my email? Matt H.<br /> <br /> FROM SPUCK - <br /> - Turn LEFT onto E 1ST ST / US-62 N. Continue to follow US-62 N. Go 2.9 miles Map <br /> <br /> - US-62 N becomes PA-157. Go 13.5 miles Map <br /> <br /> - Turn SLIGHT RIGHT onto PA-208. Go 3.7 miles Map <br /> <br /> - Turn RIGHT onto MILLERSTOWN RD. Go 1.4 miles <br /> <br /> - Gravel lane is on right hand side. Come up lane about 1000 feet.<br /> <br /> [[Image: directions.JPG|center]]<br /> <br /> <br /> <br /> How late into saturday are you planning to work saturday b/c i can't be there until like 1 o'clock earliest!! MATT W.<br /> <br /> FROM SPUCK - Is there another day that works better for everyone ... for example Monday morning July 2 into MOnday afternoon??? Please let me know what your schedule is. Also, keep in mind when you make comments that this discussion page is something that can be viewed by the entire world. This is ok, because we want other teacher/student research teams to see first hand the both the good and bad of trying to conduct student teacher research. We are kind of like the &quot;reality TV show&quot; only on the web. :) Thanks, please respond ASAP. Mr. Spuck<br /> <br /> I am gonna be gone from the July 1st to the 6th in Virginia. I was talking to Nick Kelley and he was saying that he can make it on the 30th anytime like me. Whatever time Matt W. can make the meeting is fine with me and Nick!! Also Greg is currently in Washington DC with a biology seminar and will not be back till July 3rd. He wanted me to fill him in with all the info he is gonna miss when he gets back. Matt H.<br /> <br /> FROM SPUCK - Ok ... it looks like we will meet on Saturday (June 30th). Has anyone spoken to Danni or Alexis?? So where do we want to meet and what time? I'm not sure what condition my room is at the high school because of summer cleaning. I will know more tomorrow when I go up to the school. If we meet at my place, I think we should start BY 10:00 AM and plan on going till about 5:00 PM. If your parents could bring you out, then I could get you back to the Oil City area by 6:00 PM on Saturday, or they can pick you up. Let me know what you think. Matt H. ... have you been in recent contact with Nick? Why has he not posted on the Wiki? Thanks.<br /> <br /> I have been talking to Nick about our upcoming meeting this weekend. However right now Nick is grounded and I believe he can not use the internet.(not sure totally) Also that time at your house is fine with me. Though I might have to be leaving an hour early but right now I'm not certain, I will find out tomorrow and post it up here. Also I will try to get a hold of Nick to tell him about the meeting. Matt H.<br /> <br /> SaturdaY IS THE BEST DAy for me i work 11pm to 7am sundaye night and i work 11pm 7am monday night so that wont work<br /> <br /> FROM SPUCK - I'll assume the comments above are from Nick Kelley. I'f wrong please let me know. I checked my room out yesterday at the high school and everything has been removed for cleaning. So I guess it is my house (see directions above). Plan on arriving between 9:30 and 10:00 AM and we will plan on stopping right around 5:00 PM. Either your parents could pick you up at 5:00 PM or I'll be going to Oil City around 6:00 PM on Saturday and I could give you a ride. If I have this correct it will be Nick at Matt H, with Matt W coming by in the afternoon. Anyone else?<br /> <br /> Sounds right to me... Matt W.</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:Main_Page&diff=1785 Talk:Main Page 2007-06-27T13:42:29Z <p>Mattw: /* Planning for work session June 29 and/or June 30th for Oil City Students */</p> <hr /> <div>hey this is nick Kelley from Oil City it is going to be fun working with everybody<br /> <br /> == Hello ==<br /> <br /> Hey guys this is Matt Heath from Oil City. I can not wait to work with all of you guys through this wiki.<br /> <br /> sweet<br /> <br /> ITS matt walentosky, does this work?<br /> <br /> == Planning for work session June 29 and/or June 30th for Oil City Students ==<br /> <br /> Matt, Matt, Nick, Greg, Danni, Alexis, and Sandy,<br /> <br /> We had tentatively planned to meet to work on Spitzer stuff and get ready for California on Friday June 29 and/or Saturday June 30. We could meet at the high school something that might be a bit more relaxed is to meet here at my house near Pine City. Please make comments here at the Wiki site as to what your schedule is like and whether or not you can make a work session. Please do this ASAP so we can decide what will work.<br /> <br /> Thanks, Mr. Spuck<br /> <br /> Anytime on Saturday the 30th is good for me. I can not make it on the 29th because my brother is arriving from New Jersey that day. Where exactly in Pine City do you live? Could you send directions to my email? Matt Heath<br /> <br /> FROM SPUCK - <br /> - Turn LEFT onto E 1ST ST / US-62 N. Continue to follow US-62 N. Go 2.9 miles Map <br /> <br /> - US-62 N becomes PA-157. Go 13.5 miles Map <br /> <br /> - Turn SLIGHT RIGHT onto PA-208. Go 3.7 miles Map <br /> <br /> - Turn RIGHT onto MILLERSTOWN RD. Go 1.4 miles <br /> <br /> - Gravel lane is on right hand side. Come up lane about 1000 feet.<br /> <br /> How late into saturday are you planning to work saturday b/c i can't be there until like 1 o'clock earliest!! MATT W.</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:Main_Page&diff=1784 Talk:Main Page 2007-06-27T13:41:02Z <p>Mattw: /* Planning for work session June 29 and/or June 30th for Oil City Students */</p> <hr /> <div>hey this is nick Kelley from Oil City it is going to be fun working with everybody<br /> <br /> == Hello ==<br /> <br /> Hey guys this is Matt Heath from Oil City. I can not wait to work with all of you guys through this wiki.<br /> <br /> sweet<br /> <br /> ITS matt walentosky, does this work?<br /> <br /> == Planning for work session June 29 and/or June 30th for Oil City Students ==<br /> <br /> Matt, Matt, Nick, Greg, Danni, Alexis, and Sandy,<br /> <br /> We had tentatively planned to meet to work on Spitzer stuff and get ready for California on Friday June 29 and/or Saturday June 30. We could meet at the high school something that might be a bit more relaxed is to meet here at my house near Pine City. Please make comments here at the Wiki site as to what your schedule is like and whether or not you can make a work session. Please do this ASAP so we can decide what will work.<br /> <br /> Thanks, Mr. Spuck<br /> <br /> Anytime on Saturday the 30th is good for me. I can not make it on the 29th because my brother is arriving from New Jersey that day. Where exactly in Pine City do you live? Could you send directions to my email? Matt Heath<br /> <br /> FROM SPUCK - <br /> - Turn LEFT onto E 1ST ST / US-62 N. Continue to follow US-62 N. Go 2.9 miles Map <br /> <br /> - US-62 N becomes PA-157. Go 13.5 miles Map <br /> <br /> - Turn SLIGHT RIGHT onto PA-208. Go 3.7 miles Map <br /> <br /> - Turn RIGHT onto MILLERSTOWN RD. Go 1.4 miles <br /> <br /> - Gravel lane is on right hand side. Come up lane about 1000 feet.<br /> <br /> How late into saturday are you planning to work saturday b/c i can't be there until like 1 o'clock earliest!!</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:Main_Page&diff=1783 Talk:Main Page 2007-06-27T13:37:38Z <p>Mattw: /* Planning for work session June 29 and/or June 30th for Oil City Students */</p> <hr /> <div>hey this is nick Kelley from Oil City it is going to be fun working with everybody<br /> <br /> == Hello ==<br /> <br /> Hey guys this is Matt Heath from Oil City. I can not wait to work with all of you guys through this wiki.<br /> <br /> sweet<br /> <br /> ITS matt walentosky, does this work?<br /> <br /> == Planning for work session June 29 and/or June 30th for Oil City Students ==<br /> <br /> Matt, Matt, Nick, Greg, Danni, Alexis, and Sandy,<br /> <br /> We had tentatively planned to meet to work on Spitzer stuff and get ready for California on Friday June 29 and/or Saturday June 30. We could meet at the high school something that might be a bit more relaxed is to meet here at my house near Pine City. Please make comments here at the Wiki site as to what your schedule is like and whether or not you can make a work session. Please do this ASAP so we can decide what will work.<br /> <br /> Thanks, Mr. Spuck<br /> <br /> Anytime on Saturday the 30th is good for me. I can not make it on the 29th because my brother is arriving from New Jersey that day. Where exactly in Pine City do you live? Could you send directions to my email? Matt Heath<br /> <br /> FROM SPUCK - <br /> - Turn LEFT onto E 1ST ST / US-62 N. Continue to follow US-62 N. Go 2.9 miles Map <br /> <br /> - US-62 N becomes PA-157. Go 13.5 miles Map <br /> <br /> - Turn SLIGHT RIGHT onto PA-208. Go 3.7 miles Map <br /> <br /> - Turn RIGHT onto MILLERSTOWN RD. Go 1.4 miles <br /> <br /> - Gravel lane is on right hand side. Come up lane about 1000 feet.</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:Main_Page&diff=1782 Talk:Main Page 2007-06-27T13:36:23Z <p>Mattw: </p> <hr /> <div>hey this is nick Kelley from Oil City it is going to be fun working with everybody<br /> <br /> == Hello ==<br /> <br /> Hey guys this is Matt Heath from Oil City. I can not wait to work with all of you guys through this wiki.<br /> <br /> sweet<br /> <br /> ITS matt walentosky, does this work?<br /> <br /> == Planning for work session June 29 and/or June 30th for Oil City Students ==<br /> <br /> Matt, Matt, Nick, Greg, Danni, Alexis, and Sandy,<br /> <br /> We had tentatively planned to meet to work on Spitzer stuff and get ready for California on Friday June 29 and/or Saturday June 30. We could meet at the high school something that might be a bit more relaxed is to meet here at my house near Pine City. Please make comments here at the Wiki site as to what your schedule is like and whether or not you can make a work session. Please do this ASAP so we can decide what will work.<br /> <br /> Thanks, Mr. Spuck<br /> <br /> Anytime on Saturday the 30th is good for me. I can not make it on the 29th because my brother is arriving from New Jersey that day. Where exactly in Pine City do you live? Could you send directions to my email? Matt Heath<br /> <br /> FROM SPUCK - <br /> - Turn LEFT onto E 1ST ST / US-62 N. Continue to follow US-62 N. Go 2.9 miles Map <br /> <br /> - US-62 N becomes PA-157. Go 13.5 miles Map <br /> <br /> - Turn SLIGHT RIGHT onto PA-208. Go 3.7 miles Map <br /> <br /> - Turn RIGHT onto MILLERSTOWN RD. Go 1.4 miles <br /> <br /> - Gravel lane is on right hand side. Come up lane about 1000 feet.<br /> <br /> ~If we meet saturday at your house the earliest i can be their is like 1 in the afternoon cause i have a baseball game!!!<br /> ''Matt W.''</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=Talk:Main_Page&diff=1768 Talk:Main Page 2007-06-08T18:09:06Z <p>Mattw: </p> <hr /> <div>hey this is nick Kelley from Oil City it is going to be fun working with everybody<br /> <br /> == Hello ==<br /> <br /> Hey guys this is Matt Heath from Oil City. I can not wait to work with all of you guys through this wiki.<br /> <br /> sweet<br /> <br /> ITS matt walentosky, does this work?</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=User_talk:Mattw&diff=1764 User talk:Mattw 2007-06-08T18:00:30Z <p>Mattw: </p> <hr /> <div>== Matt Walentosky =<br /> <br /> I am a student at oil city high school and i'm looking forward to working with everybody... this is going to be really fun.</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=User_talk:Mattw&diff=1761 User talk:Mattw 2007-06-08T17:48:26Z <p>Mattw: </p> <hr /> <div>== Matt Walentosky ==<br /> <br /> Hey this is matt walentosky, i am a student at oil city high school and i'm looking forward to working with everybody... this is going ti be really fun.</div> Mattw https://vmcoolwiki.ipac.caltech.edu/index.php?title=User_talk:Mattw&diff=1760 User talk:Mattw 2007-06-08T17:44:28Z <p>Mattw: Matt Walentosky</p> <hr /> <div>== Matt Walentosky ==<br /> <br /> Hey this is matt w!!</div> Mattw