Difference between revisions of "Talk:C-WAYS Spring work"
| Line 2: | Line 2: | ||
== Getman 2006 X-Ray Study of Triggered Star Formation and Protostars in IC 1396N == | == Getman 2006 X-Ray Study of Triggered Star Formation and Protostars in IC 1396N == | ||
| − | + | An observation of IC 1396N with Chandra, so X-ray light. How long (total time) was the observation? 30 ks = 30 kilo seconds = 30,000 seconds = 500 min = 8.33 hours - '''Is this a long observation? I got that impression from the reading.''' | |
Revision as of 02:55, 4 May 2012
Getman 2006 X-Ray Study of Triggered Star Formation and Protostars in IC 1396N
An observation of IC 1396N with Chandra, so X-ray light. How long (total time) was the observation? 30 ks = 30 kilo seconds = 30,000 seconds = 500 min = 8.33 hours - Is this a long observation? I got that impression from the reading.
Intro - What will be useful in this section for us?
Question
1. Is the cometary globule this study looks at BRC 38? (not sure - last week cg were defined as different than brc)
Nice list of indicators of star formation in IC 1396N. Things we should know about
-IRAS source 21391 +5802
-H2O masers
-molecular outflows
-HH flows
-clusters of IR embedded sources
-radio mm portostars (is this observations in radio?)
Explanation of RDI - easy to understand. Explanation of why an x-ray study - I was surprised. Didn't think about magnetic fields being active in YSO.
"2.1 - 2.3 Chandra Observation & Source List - The meat for us!"
The most important things here are the tables and figures. Locations given for the found sources and correlations to 2MASS. Will we eventually understand what each of these columns mean?
2.1 - Interesting that 8 corrections were made to the data. EIGHT pg 317-8 Data reduced to 117 point sources (listed in table 1); 66 of those correlated with 2MASS; 5 newly identified
Sections 3, 4 & 5 - Interesting things about IC 1396N
3.1-3.4 Data reduced to sources coming from star formation. 25 sources are probable members of the globule. Sources classified as class 0, I, II, III.
4.1- 4.3 It was interesting that there was flaring going on. Are YSO variable in the their light output, like a variable star? 4.3 was hard to understand. I have to sort out wavelengths and energies associated with each em light band.
5.1-5.3 Figure 10 a - This is a great picture of results of using different types of observations and even of resolution. Why correlation with other studies is needed. Figure 10 c - Source 66 and 68 are so much brighter than the others. Interesting. It was also interesting that #66 is the brightest x-ray object in IC 1396N. What does it mean that it is 'one of the most heavily absorbed sources'?
Questions
1. Does this symbol mean of the Sun? M⊙ = mass in relation to the Sun?
2. What is IMF - initial mass function? pg 328, last full paragraph
3. What is MedE? pg 331 5.2
4. What is intervening column density? pg 332 5.3 2nd paragraph
5. What is extinction? pg 332 5.3 3rd paragraph
"Section 6 & 7 - Science questions and summary"
Section 6 pulls the info from the study into the larger science questions - What do these results say about triggered star formation and the two initiation methods mentioned? It seems that RDI (radiation driven implosion) is supported.
I like section 7's summary. Easy to understand and I like the list of classifications of the 25 YSO.
