J/A+A/595/A80 H_2_O lines reduced spectra in 11 ULIRGs or HyLIRGs (Yang+, 2016) ================================================================================ Submillimeter H_2_O and H_2_O^+^ 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. =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 H_2_O 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 H_2_O emission lines. These include five 3_21_-3_12_ ortho-H_2_O lines (Eup/k=305K) and nine J=2 para-H_2_O lines, either 2_02_-1_11_ (E_up/k=101K) or 2_11_-2_02_ (E_up/k = 137K). The apparent luminosities of the H_2_O emission lines are {mu}L_H2O_~6-21x10^8^L_{sun}_ (3<{mu}<15, where {mu} 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 H_2_O lines are found to be similar, generally within 1{sigma} 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), H_2_O is found to be among the strongest molecular emitters in high-redshift Hy/ULIRGs. We also confirm our previously found correlation between luminosity of H_2_O (LH_2_O) and infrared (LIR) that LH_2_O~LIR^(1.1-1.2)^, with our new detections. This correlation could be explained by a dominant role of far-infrared pumping in the H_2_O excitation. Modelling reveals that the far-infrared radiation fields have warm dust temperature T_warm_~45-75K, H_2_O column density per unit velocity interval N_H2O_/{DELTA}V>~0.3x10^15^km/s/cm^2^ and 100{mu}m continuum opacity {tau}_100_>1 (optically thick), indicating that H_2_O is likely to trace highly obscured warm dense gas. However, further observations of J>=4 H_2_O lines are needed to better constrain the continuum optical depth and other physical conditions of the molecular gas and dust. We have also detected H_2_O^+^ emission in three sources. A tight correlation between L_H_2_O and L_H_2_O^+^ has been found in galaxies from low to high redshift. The velocity-integrated flux density ratio between H_2_O^+^ and H_2_O suggests that cosmic rays generated by strong star formation are possibly driving the H_2_O^+^ formation. Description: The FITS file of the 1D spectra of the H_2_O lines are presented. The data files are corresponding to Table 1 in the paper. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table1.dat 189 17 Observation log fits/* . 17 Individual fits spectra -------------------------------------------------------------------------------- Byte-by-byte Description of file: table1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 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 H_2_O 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 -------------------------------------------------------------------------------- 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) (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). -------------------------------------------------------------------------------- Acknowledgements: Chentao Yang, yangcht(at)pmo.ac.cn ================================================================================ (End) C. Yang [PMO, China, IAS/IAP France] P. Vannier [CDS] 04-Oct-2016