copy visit 1 to visit 19. HOPR copy.
----- Attempting Submission 1 (Fri Jun 20 19:56:44 GMT 2008) -----
Phase II Proposal 11728 (psb17_phase2.apt) successfully submitted.
----- Attempting Submission 2 (Tue Jun 24 21:54:23 GMT 2008) -----
Phase II Proposal 11728 (psb17_phase2.apt) successfully submitted.
----- Attempting Submission 3 (Wed Jun 25 19:44:32 GMT 2008) -----
Phase II Proposal 11728 (psb17_phase2.apt) successfully submitted.
----- Attempting Submission 4 (Mon Jun 30 21:23:07 GMT 2008) -----
----- Attempting Submission 5 (Sat Jun 06 15:54:41 GMT 2009) -----
----- Attempting Submission 6 (Fri Dec 04 13:46:24 GMT 2009) -----
----- Attempting Submission 7 (Tue Mar 16 15:18:09 GMT 2010) -----
----- Attempting Submission 8 (Wed Feb 09 16:06:13 GMT 2011) -----
Assigned ID: 567
----- Attempting Submission 1 (Fri Mar 07 20:52:35 GMT 2008) -----
Phase I Proposal 567 (psb17.apt) successfully submitted.
----- Attempting Submission 2 (Fri Mar 07 22:23:20 GMT 2008) -----
Phase I Proposal 567 (psb17.apt) successfully submitted.
----- Attempting Submission 3 (Fri Mar 07 22:59:33 GMT 2008) -----
The Impact of Starbursts on the Gaseous Halos of Galaxies
Perhaps the most important (yet uncertain) aspects of galaxy evolution are the processes by which galaxies accrete gas and by which the resulting star formation and black hole growth affects this accreting gas. It is believed that both the form of the accretion and the nature of the feedback change as a function of the galaxy mass. At low mass the gas comes in cold and the feedback is provided by massive stars. At high mass, the gas comes in hot, and the feedback is from an AGN. The changeover occurs near the mass where the galaxy population transitions from star-forming galaxies to red and dead ones. The population of red and dead galaxies is building with cosmic time, and it is believed that feedback plays an imporant role in this process: shutting down star formation by heating and/or expelling the reservoir of cold halo gas. To investigate these ideas, we propose to use COS far-UV spectra of background QSOs to measure the properties of the halo gas in a sample of galaxies near the transition mass that have undergone starbursts within the past 100 Myr to 1 Gyr. The galactic wind associated with the starburst is predicted to have affected the properties of the gaseous halo. To test this, we will compare the properties of the halos of the post-starburst galaxies to those of a control sample of galaxies matched in mass and QSO impact parameter. Do the halos of the post-starburst galaxies show a higher incidence rate of Ly-Alpha and metal absorption-lines? Are the kinematics of the halo gas more disturbed in the post-starbursts? Has the wind affected the ionization state and/or the metallicity of the halo? These data will provide fresh new insights into the role of feedback from massive stars on the evolution of galaxies, and may also offer clues about the properties of the QSO metal absorption-line systems at high-redshift
.
Observations show that the CIV absorption-line clouds seen in the spectra of background
QSOs have a covering factor of near-unity in galaxy halos out to a radius of ~160 kpc
(for H0 = 70 km s−1, Omega_M = 0.3, and Omega_Lambda = 0.7).. The CIV1548 rest equivalent widths range from 0.1 to 2 °A. Our goal is to achieve a signal-to-noise sufficient to detect the weakest such lines at better than the 4 sigma confidence level, which requires a S/N of ~15 per spectral resolution element. To estimate the required observing time we have used the COS Exposure Time Calculator (ETC). For each target we have used the GALEX FUV magnitude (1550 °A), the generic QSO spectrum supplied by the ETC, and the redshifts for each QSO and galaxy from SDSS to calculate the exposure time necessary to achieve a signal-to-noise of 15 per resolution element at the wavelength of the redshifted CIV absorption-line. The corresponding S/N per resolution element for Ly-alpha is typically 25.
The required exposure times require from one to four orbits per target. The total is 24
orbits for the post-starbursts and 10 orbits for the control sample, for a total request of 34
orbits.
ISM IN EXTERNAL GALAXIES
12
false
0.0
0.0
false
false
false
false
AVAILABLE
UNIDENTIFIED
BLR
NUCLEUS
J2000
16 19 16.5400
+33 42 38.40
J2000
FUV = 18.56
UNIDENTIFIED
BLR
NUCLEUS
J2000
08 43 49.7500
+26 19 10.80
J2000
FUV = 18.36
UNIDENTIFIED
ACCRETION DISK
BLR
J2000
13 20 59.4100
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J2000
FUV = 18.48
UNIDENTIFIED
ACCRETION DISK
BLR
J2000
12 21 15.3200
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J2000
FUV = 19.1
UNIDENTIFIED
ACCRETION DISK
BLR
J2000
12 25 34.9900
-02 47 57.10
J2000
FUV = 18.5
UNIDENTIFIED
ACCRETION DISK
BLR
J2000
23 08 45.5900
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J2000
FUV = 18.0
UNIDENTIFIED
ACCRETION DISK
BLR
J2000
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J2000
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UNIDENTIFIED
ACCRETION DISK
BLR
J2000
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J2000
FUV = 16.8
UNIDENTIFIED
ACCRETION DISK
BLR
J2000
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J2000
FUV = 18.7
UNIDENTIFIED
ACCRETION DISK
BLR
J2000
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J2000
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UNIDENTIFIED
ACCRETION DISK
BLR
J2000
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J2000
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UNIDENTIFIED
ACCRETION DISK
BLR
J2000
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UNIDENTIFIED
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UNIDENTIFIED
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J2000
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J2000
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J2000
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J2000
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UNIDENTIFIED
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UNIDENTIFIED
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J2000
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UNIDENTIFIED
ACCRETION DISK
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J2000
13 21 44.9700
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J2000
FUV=17.6
COS/FUV
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G140L
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No
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No
G140L
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COS/FUV
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No
G140L
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No
G140L
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COS/FUV
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No
G140L
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COS/FUV
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No
G140L
1230
COS/FUV
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No
No
G140L
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COS/FUV
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No
G140L
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COS/FUV
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No
G140L
1230
COS/FUV
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No
G140L
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COS/FUV
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No
No
G140L
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COS/FUV
Spectroscopic
No
No
G140L
1230
COS/FUV
Spectroscopic
No
No
G140L
1230
COS/FUV
Spectroscopic
No
No
G140L
1230
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