J/A+A/595/A80 H2O lines reduced spectra in 11 ULIRGs or HyLIRGs (Yang+, 2016)
Submillimeter H2O and H2O+ emission in lensed ultra- and hyper-luminous
infrared galaxies at z ∼ 2-4.
Yang C., Omont A., Beelen A., Gonzalez-Alfonso E., Neri R., Gao Y.,
van der Werf P., Weiss A., Gavazzi R., Falstad N., Baker A.J.,
Bussmann R.S., Cooray A., Cox P., Dannerbauer H., Dye S., Guelin M.,
Ivison R., Krips M., Lehnert M., Michalowski M.J., Riechers D.A.,
Spaans M., Valiante E.
<Astron. Astrophys. 595, A80 (2016)>
=2016A&A...595A..80Y 2016A&A...595A..80Y (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, spectra; Interstellar medium; Millimetric/submm sources
Keywords: galaxies: high-redshift - galaxies: ISM - infrared: galaxies -
submillimeter: galaxies - radio lines: ISM - ISM: molecules
Abstract:
We report rest-frame submillimeter H2O emission line observations of
11 ultra- or hyper-luminous infrared galaxies (ULIRGs or HyLIRGs) at
z∼2-4 selected among the brightest lensed galaxies discovered in the
Herschel-Astrophysical Terahertz Large Area Survey (H-ATLAS). Using
the IRAM NOrthern Extended Millimeter Array (NOEMA), we have detected
14 new H2O emission lines. These include five 321-312
ortho-H2O lines (Eup/k=305K) and nine J=2 para-H2O lines, either
202-111 (E_up/k=101K) or 211-202 (E_up/k = 137K). The apparent
luminosities of the H2O emission lines are
µLH2O∼6-21x108L☉ (3<µ<15, where µ is the lens
magnification factor), with velocity-integrated line fluxes ranging
from 4-15Jy.km/s. We have also observed CO emission lines using EMIR
on the IRAM 30m telescope in seven sources (most of those have not yet
had their CO emission lines observed). The velocity widths for CO and
H2O lines are found to be similar, generally within 1σ errors
in the same source. With almost comparable integrated flux densities
to those of the high-J CO line (ratios range from 0.4 to 1.1), H2O
is found to be among the strongest molecular emitters in high-redshift
Hy/ULIRGs. We also confirm our previously found correlation between
luminosity of H2O (LH2O) and infrared (LIR) that
LH2O∼LIR(1.1-1.2), with our new detections. This correlation could
be explained by a dominant role of far-infrared pumping in the H2O
excitation. Modelling reveals that the far-infrared radiation fields
have warm dust temperature Twarm∼45-75K, H2O column density per
unit velocity interval NH2O/{DELTA}V≳0.3x1015km/s/cm2 and
100µm continuum opacity τ100>1 (optically thick), indicating
that H2O is likely to trace highly obscured warm dense gas. However,
further observations of J≥4 H2O lines are needed to better
constrain the continuum optical depth and other physical conditions of
the molecular gas and dust. We have also detected H2O+ emission in
three sources. A tight correlation between LH2_O and LH2_O+ has
been found in galaxies from low to high redshift. The
velocity-integrated flux density ratio between H2O+ and H2O
suggests that cosmic rays generated by strong star formation are
possibly driving the H2O+ formation.
Description:
The FITS file of the 1D spectra of the H2O lines are presented. The
data files are corresponding to Table 1 in the paper.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 189 17 Observation log
fits/* . 17 Individual fits spectra
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- --- [H-ATLAS]
9- 24 A16 --- H-ATLAS H-ATLAS IAU Name (JHHMMSS.s+DDMMSS)
26- 36 A11 --- Source Source name
37 A1 --- n_Source [*] Note on G09v1.124 (1)
39- 40 I2 h RAh Source right ascension (J2000) (2)
42- 43 I2 min RAm Source right ascension (J2000) (2)
45- 49 F5.2 s RAs Source right ascension (J2000) (2)
51 A1 --- DE- Source declination peak (J2000) (2)
52- 53 I2 deg DEd Source declination peak (J2000) (2)
55- 56 I2 arcmin DEm Source declination peak (J2000) (2)
58- 62 F5.2 arcsec DEs Source declination peak (J2000) (2)
64- 65 I2 h RAPh Source right ascension (J2000) (3)
67- 68 I2 min RAPm Peak right ascension (J2000) (3)
70- 74 F5.2 s RAPs Peak right ascension (J2000) (3)
76 A1 --- DEP- Peak declination peak (J2000) (3)
77- 78 I2 deg DEPd Peak declination peak (J2000) (3)
80- 81 I2 arcmin DEPm Peak declination peak (J2000) (3)
83- 87 F5.2 arcsec DEPs Peak declination peak (J2000) (3)
89- 99 A11 --- H2O H2O line (4)
101-107 F7.3 GHz PeakObs Central observed frequency
109-111 F3.1 arcsec Beam1 Beam
112 A1 --- --- [x]
113-115 F3.1 arcsec Beam2 Beam
117-119 F3.1 h tcon On-source integration time
121-146 A26 --- FileName Name of the fits file in subdirectory fits (5)
148-189 A42 --- Title Title of the fits file
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Note (1): The source G09v1.124, which is not resolved by SPIRE, is a cluster
that consists of two main components: eastern component W (G09v1.124-W) and
western component T (G09v1.124-T) as described in Ivison et al.
(2013ApJ...772..137I 2013ApJ...772..137I) (see also Fig. A.1c).
Note (2): J2000 Herschel coordinates which were taken as the centres of the
NOEMA images displayed in Fig. A.1.
Note (3): J2000 coordinates of the NOEMA dust continuum image.
Note (4): The rest-frame frequencies of para-H2O 202-111, 211-202 and
ortho-H2O 321-312 lines are: 987.927GHz, 752.033 GHz and 1162.912GHz,
respectively (the rest-frame frequencies are taken from the JPL
catalogue: http://spec.jpl.nasa.gov).
Note (5): Each fits files contains the velocity (km/s), the flux (Jy)
and its error (Jy).
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Acknowledgements:
Chentao Yang, yangcht(at)pmo.ac.cn
(End) C. Yang [PMO, China, IAS/IAP France] P. Vannier [CDS] 04-Oct-2016