NICMOS imaging of submillimeter galaxies with CO and PAH redshifts
We propose to obtain F110W and F160W imaging of 10 z~2.4 submillimeter galaxies (SMGs) whose optical redshifts have been confirmed by the detection of millimeter CO and/or mid-infrared PAH emission. With the 4000A break falling within/between the two imaging filters, we will be able to study these sources' spatially resolved stellar populations (modulo extinction) in the rest-frame optical. SMGs' large luminosities appear to be due largely to merger-triggered starbursts; high-resolution NICMOS imaging will help us understand the stellar masses, mass ratios, and other properties of the merger progenitors, valuable information in the effort to model the mass assembly history of the universe.
NICMOS imaging of submillimeter galaxies with CO/PAH redshifts
UNRESOLVED STELLAR POPULATIONS
12
false
0.0
0.0
false
false
false
false
false
false
SUPPORTED
GALAXY
HIGH REDSHIFT GALAXY
ULTRALUMINOUS IR GAL
Coordinates from Greve et al. (2005, MNRAS, 359, 1165).
J and K magnitudes from Frayer et al. (2004, AJ, 127, 728).
J = 19.79 +/- 0.07, J-K = 2.00 +/- 0.14
J2000
02 39 52.0000
-01 35 58.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
ULTRALUMINOUS IR GAL
Coordinates from Greve et al. (2005, MNRAS, 359, 1165).
J and K magnitudes from Frayer et al. (2004, AJ, 127, 728).
J = 22.56 +/- 0.28, J-K = 3.15 +/- 0.37
J2000
04 43 7.1000
+02 10 25.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
ULTRALUMINOUS IR GAL
Coordinates from Chapman et al. (2005, ApJ, 622, 772).
J magnitude from Smail et al. (2004, ApJ, 616, 71); <J-K> = 2.6 from Frayer et al. (2004, AJ, 127, 728).
J = 20.82 +/- 0.06, J-K = 2.6 +/- 0.1
J2000
12 35 49.4000
+62 15 37.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
ULTRALUMINOUS IR GAL
Coordinates from Chapman et al. (2005, ApJ, 622, 772).
J and K magnitudes from Smail et al. (2004, ApJ, 616, 71).
J = 22.50 +/- 0.32, J-K = 2.45 +/- 0.43
J2000
12 37 7.2000
+62 14 8.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
ULTRALUMINOUS IR GAL
Coordinates from Greve et al. (2005, MNRAS, 359, 1165).
J and K magnitudes from Frayer et al. (2004, AJ, 127, 728).
J = 19.28 +/- 0.05, J-K = 1.72 +/- 0.10
J2000
14 01 4.9000
+02 52 24.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
ULTRALUMINOUS IR GAL
Coordinates from Bertoldi et al. (2000, A&A, 360, 92).
J estimated from <J-K> = 2.6 (Frayer et al. 2004, AJ, 127, 728) and K = 20.5 (Bertoldi et al. 2000).
J = 23.1 +/- 0.2; J-K = 2.6 +/- 0.1
J2000
15 41 27.8000
+66 16 17.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
ULTRALUMINOUS IR GAL
Coordinates midway between lensed images A and B (14.9" separation), based on Kneib et al. (2005, A&A, 434, 819).
J magnitude and J-K color for the sum of A+B based on Kneib et al. (2004, MNRAS, 349, 1211).
J = 21.0 +/- 0.3; J - K = 1.9 +/- 0.2
J2000
16 35 54.4830
+66 12 30.50
J2000
GALAXY
HIGH REDSHIFT GALAXY
ULTRALUMINOUS IR GAL
Coordinates from Greve et al. (2005, MNRAS, 359, 1165).
J estimated from <J-K> = 2.6 (Frayer et al. 2004, AJ, 127, 728) and K = 18.43 +/- 0.02 (Smail et al. 2004, ApJ, 616, 71).
J = 21.03 +/- 0.02, J-K = 2.6 +/- 0.1
J2000
16 36 50.4000
+40 57 34.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
ULTRALUMINOUS IR GAL
Coordinates from Greve et al. (2005, MNRAS, 359, 1165).
J estimated from <J-K> = 2.6 (Frayer et al. 2004, AJ, 127, 728) and K = 19.77 +/- 0.06 (Smail et al. 2004, ApJ, 616, 71).
J = 22.37 +/- 0.06, J-K = 2.6 +/- 0.1
J2000
16 36 58.2000
+41 05 24.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
ULTRALUMINOUS IR GAL
Coordinates from Greve et al. (2005, MNRAS, 359, 1165).
J estimated from <J-K> = 2.6 (Frayer et al. 2004, AJ, 127, 728) and K = 19.16 +/- 0.06 (Smail et al. 2004, ApJ, 616, 71).
K = 21.76 +/- 0.06, J-K = 2.6 +/- 0.1
J2000
16 37 6.5000
+40 53 14.00
J2000
GALAXY
HIGH REDSHIFT GALAXY
ULTRALUMINOUS IR GAL
Coordinates midway between lensed images A and B (14.9" separation), based on Kneib et al. (2005, A&A, 434, 819).
J magnitude and J-K color for the sum of A+B based on Kneib et al. (2004, MNRAS, 349, 1211).
J = 21.0 +/- 0.3; J - K = 1.9 +/- 0.2
J2000
16 35 54.4830
+66 12 30.50
J2000
NIC2
Imaging
No
No
F110W
NIC2
Imaging
No
No
F110W
NIC2
Imaging
No
No
F110W
NIC2
Imaging
No
No
F110W
NIC2
Imaging
No
No
F110W
NIC2
Imaging
No
No
F110W
NIC2
Imaging
No
No
F110W
NIC2
Imaging
No
No
F110W
NIC2
Imaging
No
No
F110W
NIC2
Imaging
No
No
F110W
NIC2
Imaging
No
No
F160W
NIC2
Imaging
No
No
F160W
NIC2
Imaging
No
No
F160W
NIC2
Imaging
No
No
F160W
NIC2
Imaging
No
No
F160W
NIC2
Imaging
No
No
F160W
NIC2
Imaging
No
No
F160W
NIC2
Imaging
No
No
F160W
POS-TARG
DITHER
DITHER
2.2875
NIC-XSTRIP-DITH
false
true
4
0.0
POS-TARG
NIC-SPIRAL-DITH
0.0
1
false
POS-TARG
DITHER
DITHER
1.5375
NIC-XSTRIP-DITH
false
true
4
0.0
POS-TARG
NIC-SPIRAL-DITH
0.0
2
false
POS-TARG
DITHER
0.572
LINE
0.365
false
false
74.653
4
18.528
WFC3-IR-DITHER-BOX-MIN
3
false
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true
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The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
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true
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The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
This visit targets a position midway between two lensed images of the same background galaxy (separated by 14.9" at a PA of 26.2 east of north). To keep both images away from detector edges, we (a) use the NIC2-FIX aperture, (b) use a smaller dither spacing, and (c) request that the orientation be constrained so that the line connecting the two images falls within 15 degrees of a detector *diagonal*. (The 14.9" separation was slightly underestimated in our Phase I proposal.)
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true
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The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
There will (unavoidably) be a rather bright star N642000684 in the field of view,
which has an H magnitude of 15.2 and will saturate in about 1 minute, assuming
an MOIII spectral type. ORIENT constraints have been set to make sure that the
diffraction spikes due this star do not fall on top of the target.
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true
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The scheduling data was generated by CASM 17.2.
CASM was run in Phase II mode.
This visit targets a position midway between two lensed images of the same background galaxy (separated by 14.9" at a PA of 26.2 east of north). To ensure that both images are kept away from detector edges, we use the IR-FIX aperture. Also, to avoid having a bright (H = 12.2) star fall in the corner of the field, we exclude small ranges in ORIENT.
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true
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