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CURRENT TEAMS
+ Round 6
Other EPO programs using real data
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Round 1 - AGN Spectral Energy Distributions of
GLAST Telescope Network Program Objects
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Abstract
The Gamma-Ray Large Area Space Telescope (GLAST) has a proposed
observing list that includes AGNs and Polars bright enough to be
observed optically by amateurs and students. This observing list
is maintained by the "GLAST Telescope Network" (GTN) and includes
a number of objects that have yet to be observed by the Spitzer
Space Telescope. Our project will observe one of these objects
with the Spitzer MIPS and the IRAC instruments to determine their
Spectral Energy Distribution (SED), which will be compared to a
computer model of disk emission in order to determine what component
of the SED is due to the disk and what component is due to synchrotron
radiation induced by the jets. In addition we will observe our program
objects prior to, simultaneously with, and after Spitzer observes them.
This gives a direct connection from Spitzer research to student
activities in the classroom.
Click on any teacher's name to see activities associated with NITARP.
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Technical Details
IRAC Mapping and MIPS Photometry to determine the Spectral Energy Distribution (SED)
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Target |
Instrument |
Exposure Time
wavelength in microns (u) - time in seconds |
Cycles |
Integration Time |
Total Resource Time needed |
Comments |
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GTN 7
4c 29.45 |
MIPS Photometry |
24 u = 3
70 u = 3
160 u=10
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24 u=1
70 u=1
160u=3
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24u=42s
70u=30s
160u=60s
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1110 s
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24,70 u predicted to have large signal/noise; reduced cycles to save time
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GTN 7
4c 29.45 |
IRAC Mapping |
3.6 u = 10 s
5.8 u = 10 s
4.5 u = 10 s
8.0 u = 10 s
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378.1 s
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Gaussian 5 dithering, Large Scale.
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Visibility:
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7
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4C 29.45
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11:59:31.8
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14 May 05-
27 Jun 05
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Beg. window: 81º at 8:30 PM
End window: culminates before sunset: altitude 66 º at 7:30 PM
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7
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4C 29.45
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29:14:44
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16 Dec 05-
28 Jan 06
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Beg. window: 81 º at 6:41 AM
End window: 81º at 3:40 AM
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Status: MIPS and IRAC Observed and Archived
The project was approved by the Spitzer Science Center director. He selected one of our four potential AGNs as our primary target (GTN #7, 4C 29.45) and we edited the proposal to reflect this change. After this decision, Mark Lacy reworked the AORs to refine the time needed to gather the data.
This message from Mark summarizes the change in the AOR:
..... juggled the MIPS exposure times to make sure we get a detection at 160mu (the least sensitive wavelength). I've kept the total length of the AOR almost the same (in fact it's 10s shorter), but the MIPS AOR changed
old: 24mu 3s x 3 cycles
70mu 3s x 5 cycles
160mu 3s x 5 cycles
new: 24mu 3s x 1 cycles
70mu 3s x 1 cycles
160mu 10s x 3 cycles
IRAC was fine as is.
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