Copyright © 2005 by Annual Reviews. All rights reserved
|
| Annu. Rev. Astron. Astrophys. 2005. 43:
677-725 Copyright © 2005 by Annual Reviews. All rights reserved |
Observations of the molecular gas discussed here are critical for understanding early Universe galaxy formation. The morphology, kinematics, and gas density estimates provided by better measurements of CO and other molecular lines will lead to a detailed understanding of the processes and mechanisms involved in assembling galaxies and forming stars in the early Universe.
The present suite of telescopes available for the detection of EMGs has produced a sample of 36, which is expected to grow, particularly for SMGs, within the limits of the observing time allocated for high-z CO emission searches. A doubling of the sample is not unreasonable to expect in the next five years. But this falls far short of the sample sizes needed for true statistical studies of EMG properties. The current sample is especially deficient at redshifts z > 3, where the potential of the EMGs for the study of galaxy formation is most important. There is only one EMG that probes the era of re-ionization.
Besides their limitations for the detection of more EMGs, the ability of the present telescopes to study these objects in detail is severely limited in sensitivity and angular resolution. Only the strongest sources, observed at high frequencies, possibly through gravitational lenses, and with long integration times, offer clues regarding the structure of EMGs. To understand EMGs, images that resolve and map the molecular line emitting region are critical.
ALMA is the only observing facility planned for operation within the
next decade that combines the sensitivity, angular resolution,
flexibility of observing modes, and site conditions required
for such imaging. ALMA will be the premier telescope for the study of
EMGs. Its 64
12m-diameter antennas provide the collecting area needed for high
sensitivity. The ability to reconfigure the array allows one to select
angular resolution for any observing frequency. The
angular resolution at a frequency of 350 GHz is 1" in the
compact configuration, as high as 0.014" using baselines up to the
maximum of 14 km, and scaling inversely with
frequency. The correlator can process up to 16 GHz of bandwidth from
each antenna, in four separately tunable 2-GHz-wide signals in each of
the two polarizations. The receiver noise will be
three times the quantum limit (Trx
3h
/ k) for all but the
highest frequency receiver bands. A compact
array of 12 7m-diameter antennas, plus four 12m diameter antennas
for calibration purposes, bolsters sensitivity on spatial frequencies
between that of a single 12m antenna and the shortest baseline (15m) in the
large array. The site is comparable in quality to
the South Pole for millimeter/submillimeter observing, and superbly
located for studying the southern sky and much of the northern sky. For
further information on ALMA, the reader is referred to
http://www.alma.nrao.edu/ and
http://www.eso.org/projects/alma.
Guilloteau (2001)
and
Blain (2001)
have reviewed ALMA's capability to observe high-z spectral line
and continuum emission, respectively. As an illustration of ALMA's
power for detailed studies of EMGs, consider the SMG J23099, where the
CO source has been modeled
(Genzel et al. 2003)
as a rotating disk of diameter 16 kpc
(5"). When used in a 6-km-maximum baseline configuration
(resolution 0.5") with an 8-hour integraton, ALMA will
yield an image with velocity resolution of 100 km s-1 and rms
noise of 0.4 mJy (5
).
This is 10% of the unresolved flux density of the source, enough to
check the validity of the model. Because this observation can be done
with only one of the tunable 2-GHz
inputs to the correlator, simultaneous observations of, say, CS(7-6),
HCN(4-3), and up to 29 other lines within the instantaneous bandpass of
the receiver could be made. Although these lines
may not be detected in a single 0.5" beam, the u-v data, fully
sampled to 6 km, could be smoothed to 1" resolution, thereby
yielding a 5 sensitivity
of 0.1 mJy.
For simple detection of EMGs in CO emission, the (6-5) transition, for
example, at a redshift of z = 2 with a peak line intensity of 1
mJy beam-1 (or any spectral line in the bandpass with this
peak line strength), would be seen by ALMA at the
10 level
with velocity resolution
of 50 km s-1 in a typical 4-h observing session. The continuum
emission observed in this same session at 230 GHz would reach a
5 sensitivity of 33
µJy beam-1. The continuum emission from Arp 220
moved to a redshift of z = 2 could be
detected at the 5 level in
less than 30 min of observing time. Because of the
"negative K-correction," this statement is true for Arp 220 at any redshift up to z ~ 20.
Given the sensitivity of ALMA, with seven times the collecting area of the IRAM interferometer and a superior site, it is clear that the study of EMGs will be transformed from one of imaging CO emission to one of imaging emission from a variety of interstellar molecules. The importance to gas density studies of HCN, [C I] , and [C II] have been discussed above. Carbon monosulfide may be an even better tracer of dense, star-forming gas than is HCN (Shirley et al. 2003, but its weaker lines remain beyond the reach of present telescopes. Formaldehyde is another molecule that traces dense gas, potentially accessible to ALMA observers of EMGs. Searches should be made with ALMA for the isotopomers of CO. The ALMA correlator can observe many lines simultaneously, making it very powerful for astrochemical studies.
The potential for ALMA to reveal the process of galaxy formation and evolution in the early Universe can be summarized by noting that observing CO emission in the z = 6.4 quasar SDSS J1148 tests limits of present instruments. ALMA will be able to observe CO in a galaxy at this redshift having the CO luminosity of a large, normal spiral such as M51 or NGC 891, making it possible to probe the era of re-ionization with a much larger population. Readers who wish to design their own ALMA observing programs can find a sensitivity calculator at http://www.eso.org/projects/alma/science/bin/sensitivity.html.
Other facilities will also play a significant role in the study of
EMGs. An upgraded IRAM
interferometer, the Combined Array for Research in Millimeter-wave
Astronomy (CARMA), the Submillimeter Array (SMA), and the Extended VLA
(EVLA) will add increased sensitivity and/or
bandwidth to present capability. For objects with redshift
z 
2,
CO emission from low-J levels falls in the centimeter wavelength
observing bands of the EVLA. The EVLA will be
particularly suitable for observing HCN in lower-J transitions.
Receiver systems working to wavelengths as short as 0.7 cm combined with
a powerful wide-band correlator will make the
EVLA a powerful telescope for EMG observing in the Northern
Hemisphere. Large single dishes
such as the Green Bank Telescope (GBT) are also proving useful for EMG
study, as the detection of HCN(1-0) emission in F10214
(Vanden Bout, Solomon
& Maddalena 2004)
has demonstrated. The GBT will be
primarily useful for measuring CO(1-0) luminosity, detecting new EMGs
in that line, and doing continuum surveys with 3 mm wavelength bolometer
cameras. Upon completion, the 50-m
diameter Large Millimeter Telescope (LMT) will be the most powerful
single-aperture telescope for the study of
EMGs. Its very substantial collecting area will make it a
telescope of choice for blind surveys.
The next decade will see explosive growth in the number of known EMGs, the findings concerning their properties, and most important, in knowledge of their structure and evolution. The ability of ALMA to image the kinematics of the molecular star-forming gas in galaxies from the era of recombination to the present will be invaluable to our understanding of the evolution of galaxies and the Universe.
ACKNOWLEDGEMENTS
We gratefully acknowledge the assistance of J. W. Barrett in the preparation of the figures. PVB is grateful for the hospitality of the Institut d'Astrophysique, Paris, and the Department of Astronomy, University of Texas, Austin, during the writing of this review.
| EMGa | CO coordinates | Redshift | Galaxy | Lensed? | |
| R.A. (2000) | Decl. (2000) | z(CO) | type | (µ = mag.) | |
| SMM J02396b | 02:39:56.59 | -01:34:26.6b | 1.062±0.002b | SMG | µ = 2.5b |
| Q0957+561Ac | 10:01:20.88 | +55:53:54.0d | 1.4141c | QSO | µ = 1.6, 1.7d |
| Q0957+561Bc | 10:01:21.01 | +55:53:49.4d | µ = 4.3d | ||
| HR10e | 16:45:02.26 | +46:26:26.5f | 1.439±0.001f | ERO | ? |
| IRAS F10214g | 10:24:34.56 | +47:09:09.8h | 2.28581±0.00005h | QSO | µ = 17h |
| SMM J16371b | 16:37:06.50 | +40:53:13.8b | 2.380±0.004b | SMG | ? |
| SMM J16368i | 16:36:50.43 | +40:57:34.7i | 2.3853±0.0014i | SMG | ? |
| 53W002j | 17:14:14.71 | +50:15:30.6k | 2.3927±0.0003k | Radio | Unlikely |
| SMM J16366b | 16:36:58.23 | +41:05:23.7b | 2.450±0.002b | SMG | ? |
| SMM J04431i | 04:43:07.25 | +02:10:23.3i | 2.5094±0.0002i | SMG | µ = 4.4l |
| SMM J16359Am | 16:35:54.81 | +66:12:37m | 2.5168±0.0003m | SMG | µ = 14n |
| SMM J16359Bm | 16:35:44.15 | +66:12:24m | 2.5168±0.0003m | SMG | µ = 22n |
| SMM J16359Cm | 16:35:50.85 | +66:12:06m | 2.5168±0.0003m | SMG | µ = 9n |
| Cloverleaf o | 14:15:45.97 | +11:29:43.2p | 2.5579±0.0001q | QSO | µ = 11r |
| SMM J14011s | 14:01:04.93 | +02:52:24.1t | 2.5652±0.0001t | SMG | µ=5-25t |
| VCV J1409u | 14:09:55.50 | +56:28:27.0v | 2.5832±0.0001v | QSO | ? |
| LBQS 0018z | 00:21:27.30 | -02:03:33.0u | 2.620z | QSO | ? |
| MG 0414w | 04:15:10.73 | +05:34:41.2x | 2.639±0.002w | QSO | Yesx |
| MS1512-cB58y | 14:14:22.22 | +36:36:24.8y | 2.7265±0.0005y | LBG | µ=32y |
| LBQS 1230aa | 12:33:10.47 | +16:10:53.1bb | 2.741±0.001aa | QSO | ? |
| RX J0911.4u | 09:11:27.50 | +05:50:52.0u | 2.796±0.001u | QSO | µ=22cc |
| SMM J02399dd | 02:39:51.89 | -01:35:58.8ee | 2.8076±0.0002ee | SMG | µ=2.5ee |
| SMM J04135u | 04:13:27.50 | +10:27:40.3u | 2.846±0.002u | QSO | µ=1.3ff |
| B3 J2330gg | 23:30:24.84 | +39:27:12.2gg | 3.092gg | Radio | Unlikely |
| SMM J22174b | 22:17:35.20 | +00:15:37.6b | 3.099±0.004b | SMG | ? |
| MG 0751hh | 07:51:41.46 | +27:16:31.4hh | 3.200hh | QSO | µ=17hh |
| SMM J09431i | 09:43:03.74 | +47:00:15.3i | 3.3460±0.0001i | SMG | µ=1.2ii |
| SMM J13120b | 13:12:01.20 | +42:42:08.8b | 3.408±0.002b | SMG | ? |
| TN J0121jj | 01:21:42.75 | +13:20:58.0jj | 3.520jj | Radio | ? |
| 6C1908kk | 19:08:23.70 | +72:20:11.8kk | 3.532kk | Radio | Unlikely |
| 4C60.07kk | 05:12:54.75 | +60:30:50.9ll | 3.791kk | Radio | Unlikely |
| 4C41.17Rmm | 06:50:52.24 | +41:30:31.6mm | 3.7958±0.0004mm | Radio | Unlikely |
| 4C41.17Bmm | 06:50:52.12 | +41:30:30.3mm | 3.7888±0.0008mm | ||
| APM 08279nn | 08:31:41.70 | +52:45:17.4nn | 3.9114±0.0002nn | QSO | µ=7oo |
| PSS J2322pp | 23:22:07.15 | +19:44:22.5qq | 4.1192±0.0004qq | QSO | µ=2.5rr |
| BRI 1335Nss | 13:38:03.42 | -04:32:34.1tt | 4.4074±0.0015uu | QSO | ? |
| BRI 1335S | 13:38:03.40 | -04:32:35.4tt | 4.407tt | ||
| BRI 0952aa | 09:55:00.10 | -01:30:07.1aa | 4.4337±0.0003aa | QSO | µ=4aa |
| BR 1202Nvv | 12:05:22.98 | -07:42:29.9tt | 4.6916tt | QSO | Likely |
| BR 1202Svv | 12:05:23.12 | -07:42:32.9tt | 4.6947tt | ||
| TN J0924yy | 09:24:19.92 | -22:01:41.5yy | 5.203yy | Radio | Unlikely |
| SDSS J1148ww | 11:48:16.64 | +52:51:50.3ww | 6.4189±0.0006xx | QSO | Yes |
| a Reference is to discovery paper; b Greve et al. (2004b); c Planesas et al. (1999); | |||||
| d Krips et al. (2004); e Andreani et al. (2000); f Greve, Ivison & Papadopoulos (2003); | |||||
| g Brown & Vanden Bout (1991), Solomon, Downes & Radford (1992a); h Downes & Solomon (2003); | |||||
| i Neri et al. (2003); j Scoville et al. (1997); k Alloin, Barvainis & Guilloteau (2000); | |||||
| l Smail et al. (1999); m Sheth et al. (2004); n Kneib et al. (2004b); o Barvainis et al. (1994); | |||||
| p Center of four lensed components, Kneib et al. (1998); q Barvainis et al. (1997); | |||||
| r Venturini & Solomon (2003); s Frayer et al. (1999); t Downes & Solomon (2003); | |||||
| u Hainline et al. (2004); v Beelen et al. (2004); w Barvainis et al. (1998); | |||||
| x Hewitt et al. (1992); y Baker et al. (2004); z K. Izaak, private communication; | |||||
| aa Guilloteau et al. (1999); bb Hewett et al. (1995); cc Barvainis & Ivison (2002a); | |||||
| dd Frayer et al. (1998); ee Genzel et al. (2003); ff Knudsen et al. (2003); gg De Breuck et al. (2003b); | |||||
| hh Barvainis, Alloin & Bremer (2002); ii Cowie, Barger & Kneib (2002); | |||||
| jj De Breuck, Neri & Omont (2003a); kk Papadopoulos et al. (2000); ll Greve, Ivison & Papadopoulos (2004); | |||||
| mm De Breuck et al. (2005); nn Downes et al. (1999); oo Lewis et al. (2002); pp Cox et al. (2002); | |||||
| qq Carilli et al. (2002b); rr Carilli et al. (2003); ss Guilloteau et al. (1997); tt Carilli et al. (2002b); | |||||
| uu Carilli, Menten & Yun (1999); vv Omont et al. (1996b) & Ohta et al. (1995); ww Walter et al. (2003); | |||||
| xx Bertoldi et al. (2003b); yy Klamer et al. (2005). | |||||
| EMG | Transition | S
 v |
v |
S(peak) | L'(app.) | L'(int.) | Mgas | ||||||||||
| (Jy km s-1) | (km s-1) | (mJy) | (1010 L'*)a | (1010 L'*)a | (1010
M ) |
||||||||||||
| SMM J02396 | CO 2-1b | 3.4 ± 0.3 | 780 ±60 | ~ 5 | 5.1 ± 0.5 | 2.0 | 1.6 | ||||||||||
| Q0957+561A(r) | CO 2-1c | 0.34 ± 0.06 | 160 ± 20 | 2.1 ± 0.2 | 0.9 ± 0.2 | 0.6 | 0.4 | ||||||||||
| Q0957+561A(b) | CO 2-1c | 0.25 ± 0.06 | 280 ± 60 | 0.9 ± 0.2 | 0.7 ± 0.2 | 0.4 | 0.4 | ||||||||||
| Q0957+561B | CO 2-1c | 0.61 ± 0.06 | 280 ± 50 | 2.2 ± 0.2 | 1.6 ± 0.2 | 0.4 | 0.4 | ||||||||||
| HR10 | CO 1-0d | 0.6 ± 0.1 | - | ~ 0.7 | 6.5 ± 1.1 | - | 5.2µ-1 | ||||||||||
| CO 2-1e | 1.45 | 400 | ~ 4 | 3.8 | - | ||||||||||||
| CO 5-4e | 1.35 | 380 | ~ 7 | 0.6 | - | ||||||||||||
| IRAS F10214 | CO 3-2f | 4.1 ± 0.6 | 220 ± 20 | 14.5 ± 1.5 | 11.3 ± 1.7 | 0.7 | 0.6 | ||||||||||
| 4-3f | 5.5 ± 1.0 | 220 ± 40 | 23 ± 4 | 8.6 ± 0.16 | 0.5 | ||||||||||||
| 6-5f | 8.5 ± 2.0 | 200 ± 30 | 32 ± 6 | 5.9 ± 1.4 | 0.4 | ||||||||||||
| 7-6f | 7.1 ± 2.0 | 210 ± 40 | 19 ± 5 | 3.6 ± 1.0 | 0.2 | ||||||||||||
| HCN 1-0g | 0.05 ± 0.01 | 140 ± 30 | 0.45 ± 0.08 | 2.3 ± 0.4 | 0.14 | 1.0 | |||||||||||
| [C I] 1-0h | 1.6 ± 0.2 | 160 ± 30 | 9.2 ± 1.0 | 2.1 ± 0.3 | - | ||||||||||||
| SMM J16371 | CO 3-2b | 1.0 ± 0.2 | 830 ± 130 | ~ 1 | 3.0 ± 0.6 | - | 2.4µ-1 | ||||||||||
| SMM J16368 | CO 3-2i | 2.3 ± 0.2 | 840 ± 110 | ~ 3 | 6.9 ± 0.6 | - | 5.5µ-1 | ||||||||||
| 53W002 | CO 3-2j | 1.20 ± 0.15 | 420 ± 40 | 2.5 ± 0.8 | 3.6 ± 0.4 | 3.6 | 2.9 | ||||||||||
| SMM J16366 | CO 3-2b | 1.8 ± 0.3 | 870 ± 80 | ~ 2 | 5.6 ± 0.9 | - | 4.5µ-1 | ||||||||||
| SMM J04431 | CO 3-2i | 1.4 ± 0.2 | 350 ± 60 | 3.5 ± 0.5 | 4.5 ± 0.6 | 1.0 | 0.8 | ||||||||||
| SMM J16359A | CO 3-2k | 1.6 ± 0.13 | ~ 500 | ~ 4 | 5.5 ± 0.4 | 0.4 | 0.4 | ||||||||||
| SMM J16359B | CO 3-2k | 2.50 ± 0.12 | ~ 500 | ~ 7 | 8.2 ± 0.4 | 0.4 | 0.4 | ||||||||||
| SMM J16359C | CO 3-2k | 1.58 ± 0.17 | ~ 500 | ~ 4 | 5.2 ± 0.6 | 0.6 | 0.4 | ||||||||||
| Cloverleaf | CO 3-2l | 13.2 ± 0.2 | 416 ± 6 | 30.0 ± 1.7 | 44 ± 1 | 4.0 | 3.2 | ||||||||||
| 4-3m | 21.1 ± 0.8 | 375 ± 16 | 53 ± 2 | 40 ± 2 | 3.6 | ||||||||||||
| 5-4m | 24.0 ± 1.4 | 398 ± 25 | 56 ± 3 | 29 ± 2 | 2.6 | ||||||||||||
| 7-6n | 36 ± 6 | ~ 450 | 80 ± 8 | 22 ± 4 | 2.0 | ||||||||||||
| HCN 1-0o | 0.069 ± 0.012 | ~ 300 | 0.24 ± 0.04 | 3.5 ± 0.6 | 0.32 | 2.2 | |||||||||||
| [C I] 1-0h | 3.9 ± 0.6 | 360 ± 60 | 11.2 ± 2.0 | 6.5 ± 1.0 | - | ||||||||||||
| 2-1l | 5.2 ± 0.3 | 468 ± 25 | 13.2 ± 2.9 | 3.2 ± 0.2 | - | ||||||||||||
| SMM J14011 | CO 3-2p | 2.8 ± 0.3 | 190 ± 11 | 13.2 ± 1.0 | 9.4 ± 1.0 | 0.4-1.9 | 0.3-1.5 | ||||||||||
| 7-6p | 3.2 ± 0.5 | 170 ± 30 | 12.4 ± 3.0 | 2.0 ± 0.3 | 0.08-0.4 | ||||||||||||
| [C I] 1-0h | 1.8 ± 0.3 | 235 ± 45 | 7.3 ± 1.5 | 3.0 ± 0.5 | - | ||||||||||||
| VCV J1409 | CO 3-2q | 2.3 ± 0.2 | 311 ± 28 | 6 ± 1 | 7.9 ± 0.7 | - | 6.3µ-1 | ||||||||||
| 7-6q | 4.1 ± 1.0 | ~ 300 | 10 ± 3 | 2.6 ± 0.6 | - | ||||||||||||
| 1-0r | 0.007 ± 0.002 | ~ 200 | 0.08 ± 0.03 | 0.7 ± 0.2 | - | 4.9µ-1 | |||||||||||
| LBQS 0018 | CO 3-2s | 1.55 ± 0.26 | 163 ± 29 | - | 5.4 ± 0.9 | - | 4.3µ-1 | ||||||||||
| MG0414 | CO 3-2t | 2.6 ± 0.5 | ~ 580 | 4.4 | 9.2 | - | 7.4µ-1 | ||||||||||
| MS1512-cB58 | CO 3-2u | 0.37 ± 0.08 | 175 ± 45 | ~ 2 | 1.4 ± 0.3 | 0.043 | 0.03 | ||||||||||
| LBQS 1230 | CO 3-2v | 0.80 ± 0.26 | - | - | 3.0 ± 1.0 | - | 2.4µ-1 | ||||||||||
| RX J0911.4 | CO 3-2w | 2.9 ± 1.1 | 350 ± 60 | ~ 8 | 11.3 ± 4.3 | 0.52 | 0.4 | ||||||||||
| SMM J02399 | CO 3-2x | 3.1 ±0.4 | ~ 1100 | ~ 4 | 12.2 ± 1.6 | 4.9 | 3.9 | ||||||||||
| SMM J04135 | CO 3-2w | 5.4 ± 1.3 | 340 ± 120 | ~ 16 | 22 ± 5 | 17 | 13.0 | ||||||||||
| B3 J2330 | CO 4-3y | 1.3 ± 0.3 | ~ 500 | 2.5 | 3.4 ± 0.8 | 3.4 | 2.7 | ||||||||||
| SMM J22174 | CO 3-2b | 0.8 ± 0.2 | 780 ± 100 | ~ 1 | 3.7 ± 0.9 | - | 3.0 | ||||||||||
| MG 0751 | CO 4-3z | 5.96 ± 0.45 | 390 ± 40 | ~ 15 | 16 ± 1 | 1.0 | 0.8 | ||||||||||
| SMM J09431 | CO 4-3i | 1.1 ± 0.1 | 420 ± 50 | 2.5 ± 0.5 | 3.2 ± 0.3 | 2.7 | 2.2 | ||||||||||
| SMM J13120 | CO 4-3b | 1.7 ± 0.3 | 530 ± 50 | ~ 3 | 5.2 ± 0.9 | - | 4.2µ-1 | ||||||||||
| TN J0121 | CO 4-3aa | 1.2 ± 0.4 | ~ 700 | ~ 2 | 5.4 ± 1.0 | 5.4 | 4.3 | ||||||||||
| 6C1908 | CO 4-3bb | 1.62 ± 0.30 | 530 ± 70 | ~ 3 | 5.2 ± 1.0 | 5.2 | 4.2 | ||||||||||
| 4C60.07 | CO 1-0cc | 0.15 ± 0.03 | ~ 550 | 0.27 ± 0.05 | 8.7 ± 1.7 | 8.7 | 7.0 | ||||||||||
| CO 1-0cc | 0.09 ± 0.01 | 165 ± 24 | 0.30 ± 0.10 | 5.2 ± 0.6 | 5.2 | 4.2 | |||||||||||
| 4-3bb | 1.65 ± 0.35 | ~ 550 | ~ 3 | 6.0 ± 0.9 | 6.0 | ||||||||||||
| 4-3bb | 0.85 ± 0.2 | ~ 150 | ~ 6 | 3.0 ± 0.2 | 3.0 | ||||||||||||
| 4C41.17R | CO 4-3dd | 1.20 ± 0.15 | 500 ± 100 | ~ 2.5 | 4.3 ± 0.5 | 4.3 | 5.2 | ||||||||||
| 4C41.17B | CO 4-3dd | 0.60 ± 0.15 | 500 ± 150 | ~ 1.5 | 2.2 ± 0.5 | 2.2 | 5.2 | ||||||||||
| APM 08279 | CO 1-0ee | 0.150 ± 0.045 | - | - | 9.1 ± 2.7 | 1.3 | 1.0 | ||||||||||
| 4-3ff | 3.7 ± 0.5 | 480 ± 35 | 7.4 ± 1.0 | 14 ± 2 | 2.0 | ||||||||||||
| 9-8ff | 9.1 ± 0.8 | ~ 500 | 17.9 ± 1.4 | 6.8 ± 0.6 | 1.0 | ||||||||||||
| (N/NE comp.)gg | 2-1ee | 1.15 ± 0.54 | - | - | 17 ± 8 | - | |||||||||||
| PSS J2322 | CO 1-0hh | 0.19 ± 0.08 | 200 ± 70 | 0.9 ± 0.2 | 12 ± 5 | 5.0 | 4.0 | ||||||||||
| 2-1hh | 0.92 ± 0.30 | - | 2.70 ± 0.24 | 15 ± 5 | 6.1 | ||||||||||||
| 4-3ii | 4.21 ± 0.40 | 375 ± 40 | 10.5 | 17.3 ± 1.6 | 6.9 | ||||||||||||
| 5-4ii | 3.74 ± 0.56 | 275 ± 50 | 12 | 9.8 ± 1.5 | 3.9 | ||||||||||||
| [C I] 1-0jj | 0.81 ± 0.12 | 319 ± 66 | 2.4 | 3.3 ± 0.5 | - | ||||||||||||
| BRI 1335N | CO 2-1kk | 0.18 ± 0.06 | - | 0.45 ± 0.14 | 3.3 ± 1.1 | - | 2.6µ-1 | ||||||||||
| BRI 1335S | CO 2-1kk | 0.26 ± 0.06 | - | 0.67 ± 0.14 | 4.8 ± 1.1 | - | 3.8µ-1 | ||||||||||
| BRI 1335 | CO 5-4ll | 2.8 ± 0.3 | 420 ± 60 | 6 ± 1 | 8.2 ± 0.9 | - | 6.6µ-1 | ||||||||||
| BRI 0952 | CO 5-4v | 0.91 ± 0.11 | 230 | ~ 3 | 2.8 ± 0.3 | 0.7 | 0.5 | ||||||||||
| BR 1202N | CO 2-1kk | 0.26 ± 0.05 | - | 0.44 ± 0.07 | 5.2 ± 1.0 | - | 4.2 | ||||||||||
| 5-4mm | 1.3 ± 0.3 | ~ 350 | ~ 3 | 4.2 ± 1.0 | - | ||||||||||||
| BR 1202S | CO 2-1kk | 0.23 ± 0.04 | - | 0.77 ± 0.10 | 4.6 ± 0.8 | - | 3.7 | ||||||||||
| 5-4mm | 1.1 ± 0.2 | ~ 190 | ~ 5 | 3.5 ± 0.6 | - | ||||||||||||
| BR 1202 | CO 4-3mm | 1.5 ± 0.3 | - | - | 7.6 ± 1.5 | - | 6.1 | ||||||||||
| 7-6mm | 3.1 ± 0.9 | ~ 275 | ~ 10 | 5.1 ± 1.5 | - | ||||||||||||
| TN J0924 | CO 1-0 | 0.087 ± 0.017 | ~ 300 | 0.52 ± 0.12 | 8.2 ± 1.6 | 8.2 | 6.6 | ||||||||||
| 5-4 | 1.19 ± 0.27 | ~ 300 | 7.8 ± 2.7 | 4.5 ± 1.0 | 4.5 | ||||||||||||
| SDSS J1148 | CO 3-2nn | 0.18 ± 0.04 | ~ 250 | ~ 0.6 | 2.6 ± 0.6 | - | 2.1µ-1 | ||||||||||
| 6-5oo | 0.73 ± 0.076 | ~ 280 | ~ 2.5 | 2.6 ± 0.3 | - | ||||||||||||
| 7-6oo | 0.640 ± 0.088 | ~ 280 | ~ 2.1 | 1.7 ± 0.2 | - | ||||||||||||
| a L'* = K km s-1 pc2; b Greve et al. (2004b); c Krips et al. (2003); d Greve, Ivison & Papadopoulos (2003); | |||||||||||||||||
| e Andreani et al. (2000); f D. Downes & P.M. Solomon, manuscript in preparation; | |||||||||||||||||
| g Vanden Bout, Solomon & Maddalena (2004); h Weiß et al. (2005); i Neri et al. (2003); | |||||||||||||||||
| j Alloin, Barvainis & Guilloteau (2000); k Kneib et al. (2004b); l Weiß et al. (2003); | |||||||||||||||||
| m Barvainis et al. (1997); n Kneib et al. (1998); o Solomon et al. (2003); p Downes & Solomon (2003); | |||||||||||||||||
| q Beelen et al. (2004); r Carilli et al. (2004); s K. Izaak, private communication; | |||||||||||||||||
| t Barvainis et al. (1998); u Baker et al. (2004); v Guilloteau et al. (1999); w Hainline et al. (2004); | |||||||||||||||||
| x Genzel et al. (2003); y De Breuck et al. (2003a); z Barvainis, Alloin & Bremer (2002); | |||||||||||||||||
| aa De Breuck et al. (2003b); bb Papadopoulos et al. (2000); cc Greve, Ivison & Papadopoulos (2004); | |||||||||||||||||
| dd De Breuck et al. (2005); ee Papadopoulos et al. (2001); ff Downes et al. (1999); | |||||||||||||||||
| gg Components lie 2-3" to N and NE and may be unrelated to the nuclear source; | |||||||||||||||||
| hh Carilli et al. (2002b); ii Cox et al. (2002); jj Pety et al. (2004); kk Carilli et al. (2002b); | |||||||||||||||||
| ll Guilloteau et al. (1997); mm Omont et al. (1996b); nn Walter et al. (2003); oo Bertoldi et al. (2003b). | |||||||||||||||||
| EMG | Band | Flux density | LFIR(app.) | LFIR(int.) | Mdust |
| (µm) | (mJy) | (1012
L) |
(1012
L) |
(108
M) |
|
| SMM02396 | 850 a | 11 | 16.3a | 6.5a | |
| 450 a | 42 | 16.3a | 6.5a | ||
| Q0957+561 | 850 b | 7.5±1.4 | 14c | 6c | 2.5b |
| HR10 | 1350 d | 2.13 ± 0.63 | 6.5d | 6.8µ-1 d | |
| 850 d | 4.89 ± 0.74 | 6.5d | 6.8µ-1 d | ||
| 450 d | 32.3 ± 8.5 | 6.5d | 6.8µ-1 d | ||
| 850 e | 8 ± 2 | 9e | 9µ-1 e | ||
| IRAS F10214 | 1410 f | 5.7 ± 1.0 | 60f | 3.6f | 0.23f |
| 1240 f | 10 ± 2 | 60f | 3.6f | ||
| 1230 g | 9.6 ± 1.4 | 60f | 3.6f | ||
| 1100 h | 24 ± 5 | 60f | 3.6f | ||
| 850 h | 50 ± 5 | 60f | 3.6f | ||
| 450 i | 273 ± 45 | 60f | 3.6f | ||
| 350 j | 383 ± 51 | 60f | 3.6f | ||
| SMM J16371 | 1300 k | 4.2 ± 1.1 | |||
| 850 l | 11.2 ± 2.9 | ||||
| SMM J16368 | 1300 m | 2.5 ± 0.4 | |||
| 850 n | 8.2 ± 1.7 | 16c | |||
| 53W002 | 1300 o | 1.7 ± 0.4 | |||
| SMM J16366 | 850 n | 10.7 ± 2.0 | 20c | ||
| SMM J04431 | 1300 l | 1.1 ± 0.3 | |||
| 850 p | 7.2 ± 1.7 | 13m | 3m | ||
| SMM J16359 | 1350 q | 3.0 ± 0.7 | |||
| SMM J16359A | 850 r | 11 ± 1 | 45r | 1r | 2s |
| 450 r | 45 ± 9 | 45r | 1r | 2s | |
| SMM J16359B | 850 r | 17 ± 2 | 45r | 1r | 2s |
| 450 r | 75 ± 15 | 45r | 1r | 2s | |
| SMM J16359C | 850 r | 9 ± 1 | 45r | 1r | 2s |
| 450 r | 32 ± 6 | 45r | 1r | 2s | |
| Cloverleaf | 1300 b | 18 ± 2 | 59t | 5.4t | 1.5t |
| 850 b | 58.8 ± 8.1 | 59t | 5.4t | 1.5t | |
| 450 b | 224 ± 38 | 59t | 5.4t | 1.5t | |
| 350 j | 293 ± 14 | 77j | 7j | 3.5j | |
| SMM J14011 | 1350 u | 2.5 ± 0.8 | 20u | 0.8-4.0u | 0.13-0.65v |
| 850 w | 14.6 ± 1.8 | ||||
| 450 w | 41.9 ± 6.9 | ||||
| VCV J1409 | 1300 x | 10.7 ± 0.6 | 43x | ||
| 350 y | 159 ± 14y | 35y | 38µ-1 x | ||
| LBQS 0018 | 850 z | 17.2 ± 2.9 | 33c | ||
| MG0414 | b | 40 ± 2 | |||
| 1300 b | 20.7 ± 1.3 | ||||
| 850 b | 16.7 ± 3.8 | 32c | |||
| 450 b | 66 ± 16 | ||||
| MS1512-cB58 | 1200 aa | 1.06 ± 0.35 | |||
| 850 bb | 4.2 ± 0.9 | 3.1bb | 0.1bb | ||
| LBQS 1230 | 1350 cc | 3.3 ± 0.5 | |||
| 1250 cc | 7.5 ± 1.4 | ||||
| 350 j | 104 ± 21 | 36j | 11µ-1 j | ||
| RX J0911.4 | 3000 b | 1.7 ± 0.3 | |||
| 1300 b | 10.2 ± 1.8 | ||||
| 850 b | 26.7 ± 1.4 | 51c | 2.3c | ||
| 450 b | 65 ± 19 | ||||
| 350 dd | ~ 50 | ||||
| SMM J02399 | 1270 ee | 7.0 ± 1.2 | |||
| 1350 ff | 5.7 ± 1.0 | 11 ff | 4.4 ff | 6-8 ff | |
| 850 ff | 26 ± 3 | 11 ff | 4.4 ff | 6-8 ff | |
| 750 ff | 28 ± 5 | 11 ff | 4.4 ff | 6-8 ff | |
| 450 ff | 69 ± 15 | 11 ff | 4.4 ff | 6-8 ff | |
| SMM J04135 | 850 gg | 25.0 ± 2.8 | 31 gg | 24 gg | 18 gg |
| 450 gg | 55 ± 17 | 31 gg | 24 gg | 18 gg | |
| B3 J2330 | 1200 hh | 4.8 ± 1.2 | 28 hh | 28 hh | |
| 850 ii | 14.1 ± 1.7 | 13 hh | 13 ii | ||
| 450 ii | 49 ± 18 | 13 hh | 13 ii | ||
| SMM J22174 | 850 l | 6.3 ± 1.3 | 12c | ||
| MG 0751 | 3000 jj | 4.1 ± 0.5 | |||
| 1300 jj | 6.7 ± 1.3 | ||||
| 850 b | 25.8 ± 1.3 | 49c | 2.9c | ||
| 450 b | 71 ± 15 | ||||
| SMM J09431 | 1300 m | 2.3 ± 0.4 | |||
| 850 kk | 10.5 ± 1.8 | 20m | 17m | ||
| SMM J13120 | 850 ll | 6.2 ± 1.2 | 12c | ||
| TN J0121 | 850 ii | 7.5 ± 1.0 | 7ii | 7ii | |
| 6C1908 | 850 ii | 10.8 ± 1.2 | 9.8ii | 9.8ii | |
| 4C60.07 | 1250 mm | 4.5 ± 1.2 | |||
| 850 ii | 14.4 ± 1.0 | 13ii | 13ii | ||
| 850 nn | 17.1 ± 1.3 | 32c | |||
| 450 nn | 69 ± 23 | ||||
| 4C41.17 | 1245 oo | 3.4 ± 0.7 | |||
| 850 nn | 12.1 ± 0.9 | ||||
| 450 nn | 22.5 ± 8.5 | ||||
| 350 j | 37 ± 9 | 20j | 20j | 4.6j | |
| APM 08279 | 3200 pp | 1.2 ± 0.3 | |||
| 1400 pp | 17.0 ± 0.5 | ||||
| 1300 b | 24 ± 2 | ||||
| 850 b | 84 ± 3 | ||||
| 450 b | 285 ± 11 | ||||
| 350 y | 392 ± 36 | 200y | 29y | 5.8y | |
| PSS J2322 | 1200 qq | 9.6 ± 0.5 | 9.0qq | ||
| 1350 rr | 7.5 ± 1.3 | 23 rr | 9.3 rr | ||
| 850 rr | 24 ± 2 | 23 rr | 9.3 rr | ||
| 450 rr | 79 ± 19 | 23 rr | 9.3 rr | ||
| 350 y | 66 ± 9 | 30y | 12y | 9.6y | |
| BRI 1335 | 1350 cc | 5.6 ± 1.1 | |||
| 1250 cc | 10.3 ± 1.4 | ||||
| 350 j | 52 ± 8 | 28j | 17µ-1 j | ||
| BRI 0952 | 1350 cc | 2.2 ± 0.5 | 9.6cc | 2.4cc | 0.7cc |
| 1250 cc | 2.78 ± 0.63 | ||||
| 850 b | 13.4 ± 2.3 | 25c | 6.4c | ||
| BR 1202 | 1350 cc | 16 ± 2 | |||
| 350 j | 106 ± 7 | 71j | 19j | ||
| SDSS J1148 | 1200 ss | 5.0 ± 0.6 | 25tt | 6.7µ-1 ss | |
| 850 tt | 7.8 ± 0.7 | 25tt | 2.8µ-1 tt | ||
| 450 tt | 24.7 ± 7.4 | 25tt | |||
| 350 y | 23 ± 3 | 27y | 4.4µ-1 y | ||
| a Smail et al. (2002); b Barvainis & Ivison (2002); c Using LFIR = 1.9 × 1012 S850, Neri et al. (2003); | |||||
| d Dey et al. (1999)e Greve, Ivison & Papadopoulos (1999); | |||||
| f D. Downes & P.M. Solomon, manuscript in preparation; g Downes et al. (1992); | |||||
| h Rowan-Robinson et al. (1993); i Clements et al. (1992); j Benford et al. (1999); | |||||
| k Greve et al. (2004c); l Chapman et al. (2005); m Neri et al. (2003); n Ivison et al. (2002); | |||||
| o Alloin, Barvainis & Guilloteau (2000); p Smail et al. (1999); q Kneib et al. (2004a); | |||||
| r Kneib et al. (2004b); s Sheth et al. (2004); t Weiß et al. (2003); u Downes & Solomon (2003); | |||||
| v Mean for µ = 5-25, Downes & Solomon (2003); w Ivison et al. (2000); x Omont et al. (2003); | |||||
| y A. Beelen, P. Cox, D.J. Benford, C.D. Dowell, A. Kovacs, et al., manuscript in preparation; | |||||
| z Priddey et al. (2003); aa Baker et al. (2001); bb van der Werf et al. (2001); cc Guilloteau et al. (1999); | |||||
| dd J.-W. Wu, private communication; ee Genzel et al. (2003); ff Ivison et al. (1998); | |||||
| gg Knudsen, van der Werf & Jaffe (2003); hh De Breuck et al. (2003a); ii Reuland et al. (2004); | |||||
| jj Barvainis, Alloin & Bremer (2002); kk Cowie, Barger & Kneib (2002); ll Chapman et al. (2003); | |||||
| mm Papadopoulos et al. (2000); nn Archibald et al. (2001); oo De Breuck et al. (2005); | |||||
| pp Downes et al. (1999); qq Omont et al. (2001); rr Cox et al. (2002); | |||||
| ss Bertoldi et al. (2003a); tt Robson et al. (2004). | |||||