BRC Optical Ground-Based Follow-Up - Revision history

Rebull: /* Actual observations and data reduction! */

2011-11-09T19:30:28Z

Actual observations and data reduction!

Rebull at 19:30, 9 November 2011

2011-11-09T19:30:09Z

Rebull: /* Calibration fields */

2011-09-14T20:06:36Z

Calibration fields

Rebull at 17:12, 14 September 2011

2011-09-14T17:12:51Z

Rebull at 16:26, 1 September 2011

2011-09-01T16:26:42Z

Rebull at 16:23, 1 September 2011

2011-09-01T16:23:45Z

Rebull at 16:23, 1 September 2011

2011-09-01T16:23:35Z

Rebull: /* Target brightnesses */

2011-09-01T16:19:05Z

Target brightnesses

Rebull at 16:17, 1 September 2011

2011-09-01T16:17:36Z

Rebull: /* Planning Observations */

2011-09-01T16:15:01Z

Planning Observations

← Older revision		Revision as of 19:30, 9 November 2011
Line 329:		Line 329:
	BRC 34 was observed on Oct 22, by JD Armstrong and some of his students.		BRC 34 was observed on Oct 22, by JD Armstrong and some of his students.

−	See [http://spider.ipac.caltech.edu/staff/laher/nitarp/haleakala/ \|Russ' page] for the data reduction.	+	See [http://spider.ipac.caltech.edu/staff/laher/nitarp/haleakala/ Russ' page] for the data reduction.

← Older revision		Revision as of 19:30, 9 November 2011
Line 324:		Line 324:

	UPDATE 14 Sep - [[file:brccal_peregrin.xlsx]] - file from Russ with the Sloan data that Peregrine sent for nearby Sloan calibration fields. There are two worksheets, for fields 27 and 34.		UPDATE 14 Sep - [[file:brccal_peregrin.xlsx]] - file from Russ with the Sloan data that Peregrine sent for nearby Sloan calibration fields. There are two worksheets, for fields 27 and 34.
		+
		+	=Actual observations and data reduction!=
		+
		+	BRC 34 was observed on Oct 22, by JD Armstrong and some of his students.
		+
		+	See [http://spider.ipac.caltech.edu/staff/laher/nitarp/haleakala/ \|Russ' page] for the data reduction.

← Older revision		Revision as of 20:06, 14 September 2011
Line 322:		Line 322:
	Best regards,		Best regards,
	Peregrine		Peregrine
		+
		+	UPDATE 14 Sep - [[file:brccal_peregrin.xlsx]] - file from Russ with the Sloan data that Peregrine sent for nearby Sloan calibration fields. There are two worksheets, for fields 27 and 34.

← Older revision		Revision as of 17:12, 14 September 2011
Line 290:		Line 290:
	Our working area for this aspect of our project is here: http://coolwiki.ipac.caltech.edu/index.php/BRC_Optical_Ground-Based_Follow-Up		Our working area for this aspect of our project is here: http://coolwiki.ipac.caltech.edu/index.php/BRC_Optical_Ground-Based_Follow-Up
	Near the bottom of that page, there are some airmass calculations and DSS finding charts in jpg and FITS.		Near the bottom of that page, there are some airmass calculations and DSS finding charts in jpg and FITS.
		+
		+	==Calibration fields==
		+
		+	(From Luisa, 14 Sep):
		+	Here is what my friend Peregrine found for us in regards to nearby Sloan calibration fields. There are some pretty nearby Sloan stripes that work, and our expected brightnesses are well-matched to the regime where Sloan gets good photometry.
		+
		+	He (Peregrine) also provided fits binary tables of the photometry -- we'll need this to be able to calibrate our data!
		+
		+	Note that the Sloan data are in AB mags, not Vega mags. Most Sloan folks work in AB mags
		+	instead. For AB mags, instead of a Vega zero point, you always use a flat reference spectrum,
		+	so the zero point is 3631 Jy for all bands. [[Central wavelengths and zero points\|Marginally more information here]].
		+
		+	I've forwarded this to JD, who will let us know what happens next.
		+
		+	Note from Peregrine:
		+
		+	Hi Luisa,
		+
		+	Here are the SDSS photometry for point sources in the two calibration fields. I have applied standard QA checks (rejected sources flagged as BRIGHT, EDGE, SATURATED, MOVED, or TOO_FEW_GOOD_DETECTIONS) and used a SNR > 20 cut in r, i, and z.
		+
		+	Field (ra,dec) ra dec Nsrcs
		+	BRCCAL27 (114,-11) 113.9 to 114.1 -11.1 to -10.9 412
		+	BRCCAL34 (310,+58) 309.8 to 310.2 +57.9 to +58.1 314
		+
		+	The fields that are probably of the most interest to you are:
		+	*ra
		+	*dec
		+	*psfMag_r
		+	*psfMag_i
		+
		+	Best regards,
		+	Peregrine

← Older revision		Revision as of 16:26, 1 September 2011
Line 267:		Line 267:
	John calculated brightnesses using 'option 1' above. He writes: "If I am doing it correctly I have V magnitudes for M0 ranging from around 15 to 19. 60% are brighter than magnitude 18 and 85% brighter than 19 which is what was quoted as our limit. R and I should be somewhat brighter."		John calculated brightnesses using 'option 1' above. He writes: "If I am doing it correctly I have V magnitudes for M0 ranging from around 15 to 19. 60% are brighter than magnitude 18 and 85% brighter than 19 which is what was quoted as our limit. R and I should be somewhat brighter."

−	==Note to JD==	+	==Note to JD (1 Sep 11)==

@@ Line 288: / Line 288: @@
 If you would like to talk to all of us at once, we have a weekly telecon at 3:45 pacific time on Wednesdays.
-Our working area for this aspect of our project is here:
+Our working area for this aspect of our project is here: http://coolwiki.ipac.caltech.edu/index.php/BRC_Optical_Ground-Based_Follow-Up
 Near the bottom of that page, there are some airmass calculations and DSS finding charts in jpg and FITS.

@@ Line 173: / Line 173: @@
 =More concrete observation plans!=
-=When can we observe? Hourly almanac (airmasses) for our targets=
+==When can we observe? Hourly almanac (airmasses) for our targets==
 calculated for Hawaii.
@@ Line 259: / Line 259: @@
 00    16 00     7 17     9 44   (down)    32.1     -4.8    54.1
-=Target brightnesses=
+==Target brightnesses==
 DSS images for planning purposes: [[image:brc27_dss.jpg]] and [[file:brc27_dss.fits]]
@@ Line 266: / Line 266: @@
 John calculated brightnesses using 'option 1' above.  He writes: "If I am doing it correctly I have V magnitudes for M0 ranging from around 15 to 19. 60% are brighter than magnitude 18 and 85% brighter than 19 which is what was quoted as our limit.  R and I should be somewhat brighter."

← Older revision		Revision as of 16:17, 1 September 2011
Line 170:		Line 170:

	We're still assuming no reddening. That's still almost certainly going to affect what fraction of stars we actually do detect. We can redden the model and check, but I am worried that this will be a lot of trouble for you, for not a lot of gain. In some cases, the combination of even just J, H, and K will clearly indicate some degree of reddening (e.g., the unreddened model will be a poor fit when you make the plot to check the fit).		We're still assuming no reddening. That's still almost certainly going to affect what fraction of stars we actually do detect. We can redden the model and check, but I am worried that this will be a lot of trouble for you, for not a lot of gain. In some cases, the combination of even just J, H, and K will clearly indicate some degree of reddening (e.g., the unreddened model will be a poor fit when you make the plot to check the fit).
		+
		+	=More concrete observation plans!=
		+
		+	=When can we observe? Hourly almanac (airmasses) for our targets=
		+
		+	calculated for Hawaii.
		+
		+	* Hourly airmass for brc27 *
		+	Epoch 2000.00: RA 7 04 00.0, dec -11 22 55
		+	Epoch 2011.87: RA 7 04 33.4, dec -11 24 01
		+	At midnight: UT date 2011 Nov 16, Moon 0.72 illum, 31 degr from obj
		+	Local UT LMST HA secz par.angl. SunAlt MoonAlt
		+	18 00 4 00 21 18 -9 47 (down) -71.1 -4.8 ...
		+	19 00 5 00 22 18 -8 47 (down) -73.4 ... ...
		+	20 00 6 00 23 18 -7 47 (down) -73.5 ... ...
		+	21 00 7 00 0 18 -6 46 (down) -72.2 ... ...
		+	22 00 8 00 1 18 -5 46 (v.low) -69.9 ... -1.6
		+	23 00 9 00 2 18 -4 46 4.439 -66.3 ... 11.5
		+	0 00 10 00 3 19 -3 46 2.261 -61.0 ... 24.8
		+	1 00 11 00 4 19 -2 46 1.602 -52.8 ... 38.4
		+	2 00 12 00 5 19 -1 46 1.318 -40.0 ... 52.1
		+	3 00 13 00 6 19 -0 45 1.195 -19.8 ... 65.9
		+	4 00 14 00 7 19 0 15 1.172 6.7 ... 79.6
		+	5 00 15 00 8 19 1 15 1.240 30.7 ... 84.8
		+	6 00 16 00 9 20 2 15 1.430 47.0 -7.7 71.6
		+	At midnight: UT date 2011 Dec 16, Moon 0.67 illum, 51 degr from obj
		+	Local UT LMST HA secz par.angl. SunAlt MoonAlt
		+	18 00 4 00 23 16 -7 49 (down) -73.5 -4.0 ...
		+	19 00 5 00 0 16 -6 48 (down) -72.3 -17.1 ...
		+	20 00 6 00 1 16 -5 48 (v.low) -70.0 ... ...
		+	21 00 7 00 2 16 -4 48 4.599 -66.5 ... ...
		+	22 00 8 00 3 17 -3 48 2.297 -61.2 ... ...
		+	23 00 9 00 4 17 -2 48 1.616 -53.2 ... 2.1
		+	0 00 10 00 5 17 -1 48 1.324 -40.5 ... 15.7
		+	1 00 11 00 6 17 -0 47 1.197 -20.6 ... 29.4
		+	2 00 12 00 7 17 0 13 1.171 5.7 ... 42.9
		+	3 00 13 00 8 17 1 13 1.236 30.0 ... 56.0
		+	4 00 14 00 9 18 2 13 1.420 46.6 ... 67.7
		+	5 00 15 00 10 18 3 13 1.830 57.0 ... 74.2
		+	6 00 16 00 11 18 4 13 2.884 63.7 -11.5 69.5
		+
		+
		+	* Hourly airmass for brc34 *
		+	Epoch 2000.00: RA 21 33 30.0, dec +58 04 32
		+	Epoch 2011.62: RA 21 33 50.9, dec +58 07 39
		+	At midnight: UT date 2011 Aug 16, Moon 0.93 illum, 61 degr from obj
		+	Local UT LMST HA secz par.angl. SunAlt MoonAlt
		+	19 00 5 00 16 15 -5 19 2.653 -87.8 -3.0 ...
		+	20 00 6 00 17 15 -4 19 1.997 -100.9 -16.4 -1.4
		+	21 00 7 00 18 15 -3 18 1.639 -115.3 ... 12.4
		+	22 00 8 00 19 16 -2 18 1.434 -131.9 ... 26.2
		+	23 00 9 00 20 16 -1 18 1.322 -151.3 ... 39.8
		+	0 00 10 00 21 16 -0 18 1.277 -173.2 ... 52.9
		+	1 00 11 00 22 16 0 42 1.288 164.1 ... 64.6
		+	2 00 12 00 23 16 1 42 1.359 143.1 ... 71.8
		+	3 00 13 00 0 16 2 43 1.504 124.9 ... 69.1
		+	4 00 14 00 1 17 3 43 1.760 109.2 ... 59.1
		+	5 00 15 00 2 17 4 43 2.212 95.4 -14.8 46.5
		+	6 00 16 00 3 17 5 43 3.080 82.7 -1.4 33.2
		+	At midnight: UT date 2011 Sep 16, Moon 0.86 illum, 66 degr from obj
		+	Local UT LMST HA secz par.angl. SunAlt MoonAlt
		+	19 00 5 00 18 17 -3 17 1.631 -115.8 -9.2 ...
		+	20 00 6 00 19 17 -2 16 1.430 -132.5 ... ...
		+	21 00 7 00 20 18 -1 16 1.320 -151.9 ... 6.6
		+	22 00 8 00 21 18 -0 16 1.276 -173.9 ... 20.0
		+	23 00 9 00 22 18 0 44 1.289 163.4 ... 33.6
		+	0 00 10 00 23 18 1 44 1.362 142.5 ... 47.4
		+	1 00 11 00 0 18 2 44 1.510 124.3 ... 61.3
		+	2 00 12 00 1 18 3 45 1.771 108.8 ... 75.2
		+	3 00 13 00 2 19 4 45 2.232 95.0 ... 87.5
		+	4 00 14 00 3 19 5 45 3.119 82.3 ... 76.4
		+	5 00 15 00 4 19 6 45 5.239 70.0 -17.1 62.6
		+	6 00 16 00 5 19 7 45 14.754 57.7 -3.1 48.8
		+	At midnight: UT date 2011 Oct 16, Moon 0.84 illum, 79 degr from obj
		+	Local UT LMST HA secz par.angl. SunAlt MoonAlt
		+	18 00 4 00 19 15 -2 18 1.435 -131.9 -1.2 ...
		+	19 00 5 00 20 16 -1 18 1.323 -151.2 -15.2 ...
		+	20 00 6 00 21 16 -0 18 1.277 -173.2 ... ...
		+	21 00 7 00 22 16 0 42 1.288 164.2 ... 4.2
		+	22 00 8 00 23 16 1 42 1.358 143.1 ... 17.1
		+	23 00 9 00 0 16 2 42 1.503 124.9 ... 30.3
		+	0 00 10 00 1 16 3 43 1.759 109.3 ... 43.6
		+	1 00 11 00 2 17 4 43 2.211 95.5 ... 57.2
		+	2 00 12 00 3 17 5 43 3.076 82.7 ... 70.8
		+	3 00 13 00 4 17 6 43 5.122 70.4 ... 84.0
		+	4 00 14 00 5 17 7 43 13.931 58.1 ... 81.2
		+	5 00 15 00 6 17 8 43 (down) 45.4 ... 67.7
		+	6 00 16 00 7 17 9 44 (down) 32.1 -4.8 54.1
		+
		+	=Target brightnesses=
		+
		+	John calculated these using 'option 1' above. He writes: "If I am doing it correctly I have V magnitudes for M0 ranging from around 15 to 19. 60% are brighter than magnitude 18 and 85% brighter than 19 which is what was quoted as our limit. R and I should be somewhat brighter."
		+
		+	DSS images for planning purposes: [[image:brc27_dss.jpg]] and [[file:brc27_dss.fits]]
		+	and [[image:brc34_dss.jpg]] and [[file:brc34_dss.fits]]

@@ Line 29: / Line 29: @@
 **JD says "magnitude 19 is easily within reach."
 **What are the brightnesses we expect from our targets? Ah, this is the meat of it! More below.
 *How many '''dithers''' will be needed?
 **Typically, one does at least 3 dithers in order to clean out cosmic rays, but if the exposures are very short, just one can be sufficient. It depends on how much our total integration time works out to be.
@@ Line 46: / Line 47: @@
 *What will we do with the data when we have it?
 **See the CG4 paper for examples!
 =Brightness Estimations For Our Targets=