New version with line-dither + dither box on CVZ objects, after discussions with Ken Sembach.
Visit 12 changed to CVZ, with ORIENT removed, though not clear if actually scheduable.
----- Submission 1 (Sat May 13 18:33:22 GMT 2006) -----
Phase II Proposal 10813 (mg2) successfully submitted.
----- Submission 2 (Fri Jul 28 02:14:59 GMT 2006) -----
Still an issue as to whether visit 12 can be scheduled in CVZ. If not, the ORIENT will need to be
reinstated and the secondary (dither box) pattern used instead.
Assigned ID: 509
----- Submission 1 (Sat Jan 28 00:58:25 GMT 2006) -----
MgII Absorption Line Systems: Galaxy Halos or the Metal-Enriched IGM?
MgII QSO absorption lines detected in the spectra of background QSOs were used over a decade ago to infer that all redshift z > 0.2 galaxies have gaseous halos of radius ~ 60 kpc. The actual size of the halo was believed to be proportional to the luminosity of the galaxy. However, these conclusions are now much harder to understand in light of the results from numerical simulations which show how gas evolves in the universe. These models predict that gas and galaxies merely share the same filamentary structures defined by dark matter. If these models are correct, how are MgII systems and galaxies really related? We can better understand the distribution of absorbing gas if we FIRST select galaxies close to QSO sightlines and THEN search for MgII absorption at the redshift of the intervening galaxies. This is the antithesis of the original experiments which sought to find absorbing galaxies based on known MgII systems. The frequency with which we detect MgII lines from randomly selected galaxies should enable us to better understand if absorption arises in the halos of individual galaxies, or if MgII merely arises in the same IGM that galaxies inhabit.
We have used ground-based telescopes to indentify twenty z = 0.31-0.55 galaxies within 14-51 kpc of a g < 20 QSO, and to search for MgII absorption at the galaxies' redshifts. Surprisingly, we find that only 50% of our QSOs show MgII absorption. In this proposal, we seek multi-color ACS images of twelve of the fields to i) correlate the incidence of MgII with galaxy morphology; ii) determine if absorption (or lack thereof) is related to galaxy disks or halos; iii) search for signs of galaxy interactions which may explain the large cross-sections of MgII systems; and iv) look for faint interloping galaxies closer to the line of sight than the one we identified. An important component of the program is to observe each field in the SDSS g-, r- and i-bands, to permit an estimate of the photometric redshift of any objects which lie closer to the QSO sightline than the identified galaxy, and which might actually be responsible for the absorption.
The pointing of the ACS WFCCENTER aperture is selected in such a way as to
place the QSO-galaxy pairs away from the chip gap and closer to the center of
a chip (ususally WFC1). This ensures that the chip gap never
comes close to the area between QSO and galaxy, and that the chip gap stays
away from the area around the QSO-galaxy pair, which may contain other
companion (group) galaxies.
For each field, we used the VTT and Guide Star Catalog 2 DSS images to
reposition the pair so that other (very faint) galaxies might be included in
the image, while still allowing a large range of suitable ORIENT angles to be
retained. (The ORIENT angles were read directly from the VTT.) Hence, the
Target Name given in this phase 2 is the official SDSS name for the QSO of the
QSO-galaxy pair, but the Target position itself in not that of the QSO, but of
these selected co-ordinates.
Eleven of the twelve fields are dithered using the standard ACS-WFC-DITHER-BOX
and default settings. One field (Target 10) is available in the CVZ, and for this we
use the SPIRAL pattern with nine pointings in order to fill the CVZ but also
keep the individual sub exposures similar in length to the non-CVZ orbits
(450-550 sec). POINT-SPACING and PATTERN-ORIENTATION are taken from the
ACS-WFC-DITHER-BOX parameters.
QUASAR ABSORPTION LINES AND IGM
12
false
0.0
false
false
false
false
false
SUPPORTED
EXT-MEDIUM
ABSORPTION LINE SYSTEM - EXTRAGALACTIC
u=19.8,g=19.4,r=19.2,i=19.0
J2000
00 47 45.8300
-00 00 32.60
J2000
EXT-MEDIUM
ABSORPTION LINE SYSTEM - EXTRAGALACTIC
u=20.2,g=19.7,r=19.2,i=18.7
J2000
01 29 14.0800
+01 14 26.80
J2000
EXT-MEDIUM
ABSORPTION LINE SYSTEM - EXTRAGALACTIC
u=18.9,g=18.7,r=18.5,i=18.6
J2000
01 59 0.5200
-00 48 37.90
J2000
EXT-MEDIUM
ABSORPTION LINE SYSTEM - EXTRAGALACTIC
u=20.5,g=20.1,r=19.7,i=19.3
J2000
02 50 2.4900
-08 24 13.00
J2000
EXT-MEDIUM
ABSORPTION LINE SYSTEM - EXTRAGALACTIC
u=19.6,g=19.3,r=18.9,i=18.8
J2000
07 34 58.6100
+37 14 42.90
J2000
EXT-MEDIUM
ABSORPTION LINE SYSTEM - EXTRAGALACTIC
u=19.6,g=19.5,r=19.3,i=19.3
J2000
08 34 56.6100
+47 40 2.00
J2000
EXT-MEDIUM
ABSORPTION LINE SYSTEM - EXTRAGALACTIC
u=19.3,g=19.2,r=19.0,i=19.1
J2000
09 10 40.6100
+53 54 30.50
J2000
EXT-MEDIUM
ABSORPTION LINE SYSTEM - EXTRAGALACTIC
u=19.2,g=18.8,r=18.4,i=18.2
J2000
09 12 13.2500
+53 32 14.70
J2000
EXT-MEDIUM
ABSORPTION LINE SYSTEM - EXTRAGALACTIC
u=18.2,g=18.2,r=18.1,i=18.1
J2000
09 21 50.0900
+52 58 37.70
J2000
EXT-MEDIUM
ABSORPTION LINE SYSTEM - EXTRAGALACTIC
u=18.4,g=18.3,r=18.1,i=18.1
J2000
11 27 20.2000
+65 41 37.20
J2000
EXT-MEDIUM
ABSORPTION LINE SYSTEM - EXTRAGALACTIC
u=19.0,g=19.0,r=18.9,i=18.6
J2000
11 38 53.7400
+63 29 34.90
J2000
EXT-MEDIUM
ABSORPTION LINE SYSTEM - EXTRAGALACTIC
u=19.7,g=19.1,r=19.1,i=18.9
J2000
23 40 20.4200
+00 56 2.10
J2000
ACS/WFC
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ACS/WFC
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ACS/WFC
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F775W
POS-TARG
DITHER
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LINE
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false
false
69.05
4
20.67
ACS-WFC-DITHER-BOX
1
false
POS-TARG
DITHER
DITHER
4
2.994
This is the new pattern for the CVZ objects
ACS-WFC-DITHER-BOX
false
69.07
false
0.185
0.264
2
85.27
POS-TARG
ACS-WFC-DITHER-LINE
20.86
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