J/A+A/604/A53  ALLSMOG final data release. A new APEX CO survey  (Cicone+, 2017)
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The final data release of ALLSMOG:
a survey of CO in typical local low-M_*_ star-forming galaxies.
    Cicone C., Bothwell M., Wagg J., Moller P., De Breuck C., Zhang Z.,
    Martin S., Maiolino R., Severgnini P., Aravena M., Belfiore F., Espada D.,
    Flutsch A., Impellizzeri V., Peng Y., Raj M.A., Ramirez-Olivencia N.,
    Riechers D., Schawinski K.
   <Astron. Astrophys., 604, A53 (2017)>
   =2017A&A...604A..53C    (SIMBAD/NED BibCode)
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ADC_Keywords: Galaxies, nearby ; Abundances ; Carbon monoxide
Keywords: galaxies: ISM - galaxies: general - galaxies: star formation

Abstract:
    We present the final data release of the APEX low-redshift legacy
    survey for molecular gas (ALLSMOG), comprising CO(2-1) emission line
    observations of 88 nearby, low-mass (10^8.5^<M_*_[M_{sun}_]<10^10^)
    star-forming galaxies carried out with the 230GHz APEX-1 receiver on
    the APEX telescope. The main goal of ALLSMOG is to probe the molecular
    gas content of more typical and lower stellar mass galaxies than have
    been studied by previous CO surveys. We also present IRAM 30m
    observations of the CO(1-0) and CO(2-1) emission lines in nine
    galaxies aimed at increasing the M_*_<10^9^M_{sun}_ sample size.In
    this paper we describe the observations, data reduction and analysis
    methods and we present the final CO spectra together with archival HI
    21cm line observations for the entire sample of 97 galaxies. At the
    sensitivity limit of ALLSMOG, we register a total CO detection rate of
    47%. Galaxies with higher M_*_, SFR, nebular extinction (A_V_),
    gas-phase metallicity (O/H), and HI gas mass have systematically
    higher CO detection rates.In particular, the parameter according to
    which CO detections and non-detections show the strongest statistical
    differences is the gas-phase metallicity, for any of the five
    metallicity calibrations examined in this work. We investigate scaling
    relations between the CO(1-0) line luminosity (L'_CO(1-0)_) and
    galaxy-averaged properties using ALLSMOG and a sub-sample of COLD GASS
    for a total of 185 sources that probe the local main sequence (MS) of
    star-forming galaxies and its +/-0.3dex intrinsic scatter from
    M_*_=10^8.5^M_{sun}_ to M_*_=10^11^M_{sun}_. L'_CO(1-0)_ is most
    strongly correlated with the SFR, but the correlation with M_*_ is
    closer to linear and almost comparably tight. The relation between
    L'_CO(1-0)_ and metallicity is the steepest one, although deeper CO
    observations of galaxies with A_V_<0.5mag may reveal an as much steep
    correlation with A_V_. Our results suggest that star-forming galaxies
    across more than two orders of magnitude in M_*_ obey similar scaling
    relations between CO luminosity and the galaxy properties examined in
    this work. Besides SFR, the CO luminosity is likely most fundamentally
    linked to M_*_, although we note that stellar mass alone cannot
    explain all of the variation in CO emission observed as a function of
    O/H and M_HI_.

Description:
    ALLSMOG is an ESO Large Programme for the Atacama Pathfinder
    EXperiment (APEX, project no.: E-192.A-0359, principal investigator
    (PI): J. Wagg) targeting the CO(2-1) emission line (rest frequency,
    {nu}_CO(2-1)_=230.538GHz) in 88 local, low-M* star-forming
    galaxies. The project was initially allocated 300h of ESO observing
    time over the course of four semesters, corresponding to 75h per
    semester throughout periods P92-P95 (October 2013 - September 2015).
    However, during P94 and P95 there was a slowdown in ALLSMOG
    observations, mainly due the installation of the visiting instrument
    Supercam in combination with better-than-average weather conditions
    - causing other programmes requiring more stringent precipitable
    water vapour (PWV) constraints to be prioritised. Because of the
    resulting ~50% time loss for ALLSMOG during two semesters, the ESO
    observing programmes committee (OPC) granted a one-semester extension
    of the project, hence allowing us to complete the survey in P96 (March
    2016). The final total APEX observing time dedicated to ALLSMOG
    amounts to 327h, including the overheads due to setup and calibration
    but not accounting for possible additional time lost because of
    technical issues.

    In 2014 a northern component of the ALLSMOG survey was approved at the
    IRAM 30m telescope (project code: 188-14, PI: S. Martin), aimed at
    observing the CO(1-0) (rest frequency, {nu}_CO(1-0)_=115.271GHz)
    and CO(2-1) emission lines in a sample of nine additional galaxies
    characterised by stellar masses, M*<10^9^M_{sun}_. A total of 22h of
    observations were obtained with the IRAM 30m during two observing
    runs in November 2014 and May 2015.

File Summary:
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 FileName      Lrecl  Records   Explanations
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ReadMe            80        .   This file
tablec1.dat       71       99   Details of the CO observations
tablec2.dat       61       98   CO luminosity values
tablec3.dat       67       97   Physical properties of the ALLSMOG galaxy
                                 sample - Part I
tablec4.dat       69       97   Physical properties of the ALLSMOG galaxy
                                 sample - Part II
tablec5.dat      115       97   HI gas masses
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Byte-by-byte Description of file: tablec1.dat
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   Bytes Format Units     Label   Explanations
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   1-  2  A2    ---       Samp    [A I1 I2] Sample (G1)
   4-  5  I2    ---       Seq     [1/97] ALLSMOG sequential number
   7- 23  A17   ---       Name    Galaxy name
  25- 27  I3    min       tON     ?=- On-source time (1)
  29- 32  F4.1  mJy       rms     ?=- 1{sigma} spectral rms calculated in
                                   channels of {delta}v=50km/s
  34- 37  I4    km/s      v0      ?=- Central velocity of the CO emission line
                                   with respect to the optical redshift (2)
  39- 40  I2    km/s    e_v0      ? rms uncertainty on v0
  44- 46  I3    km/s      sigma   ?=- Velocity dispersion of the observed CO
                                   line derived through a single-Gaussian
                                   fitting
  48- 49  I2    km/s    e_sigma   ? rms uncertainty on sigma
  53- 55  I3    mJy       Speak   ?=- Amplitude of the Gaussian function fitted
                                   to the observed CO line profile
  57- 59  I3    mJy     e_Speak   ? rms uncertainty on Speak
      61  A1    ---     l_Int     3{sigma} upper limit flag on Int (3)
  62- 66  F5.1  Jy.km/s   Int     Total total velocity-integrated flux of the
                                   Gaussian function fitted to the observed CO
                                   line profile
  68- 71  F4.1  Jy.km/s e_Int     ? rms uncertainty on  Int
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Note (1): For the IRAM 30m CO(1-0) observations the "human" on source time is
  half the value listed in the table, because the EMIR receiver allows
  simultaneous dual-polarisation observations that were averaged together to
  produce the final spectrum.
Note (2): central velocity of the CO emission line with respect to the optical
  redshift (inferred from SDSS observations) as derived through a
  single-Gaussian fitting.
Note (3): For the non-detections, we list the 3{sigma}-upper limit on the total
   integrated CO flux derived using Eq. (3).
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Byte-by-byte Description of file: tablec2.dat
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   Bytes Format Units            Label  Explanations
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   1-  2  A2    ---              Samp   [A I1 I2] Sample (G1)
   4-  5  I2    ---              Seq    ALLSMOG sequential number
   7- 23  A17   ---              Name   Galaxy name
  24- 29  F6.4  ---              Beam   Fraction of the expected total CO flux
                                         recovered by the beam of the
                                         single-dish telescope (1)
  31- 36  F6.4  ---            e_Beam   rms uncertainty on Beam
      38  A1    ---            l_Int    Limit flag on Int
  39- 43  F5.1  Jy.km/s          Int    Total velocity-integrated CO flux
                                         corrected for beam coverage)
  46- 49  F4.1  Jy.km/s        e_Int    ? rms uncertainty on Int
      51  A1    ---            l_L'CO   Limit flag on L'CO
  52- 56  F5.2 10+8K.km/s.pc+2   L'CO   CO line luminosity calculated from the
                                         aperture-corrected CO flux listed in
                                         Int by using Eq. (8) of the paper
  58- 61  F4.2 10+8K.km/s.pc+2 e_L'CO   ? rms uncertainty on L'CO
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Note (1): calculated as explained in Sect. 3.5 following the same method as
  Bothwell et al. (2014MNRAS.445.2599B).
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Byte-by-byte Description of file: tablec3.dat
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   Bytes Format Units   Label     Explanations
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   1-  2  A2    ---     Samp      [A I1 I2] Sample (G1)
   4-  5  I2    ---     Seq       ALLSMOG sequential number
   7- 23  A17   ---     Name      Galaxy name
  24- 25  I2    h       RAh       Right ascension (J2000)
  27- 28  I2    min     RAm       Right ascension (J2000)
  30- 34  F5.2  s       RAs       Right ascension (J2000)
      36  A1    ---     DE-       Declination sign (J2000)
  37- 38  I2    deg     DEd       Declination (J2000)
  40- 41  I2    arcmin  DEm       Declination (J2000)
  43- 44  I2    arcsec  DEs       Declination (J2000)
  46- 51  F6.4  ---     zopt      Optical spectroscopic redshift extracted from
                                   the MPA-JHU catalogue (1)
  53- 57  F5.1  Mpc     DL        Luminosity distance according to the
                                   adopted Cosmology
  59- 62  F4.1  deg     i         Inclination of the optical disk (2)
  64- 67  F4.1  arcsec  d25       Optical diameter as defined by the 25th
                                   magnitude B-band isophote (2)
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Note (1): Further details are given in Sect. 4.1
Note (2): Both i and d25 are drawn from the Hyperleda database.
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Byte-by-byte Description of file: tablec4.dat
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   Bytes Format Units      Label     Explanations
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   1-  2  A2    ---        Samp      [A I1 I2] Sample (G1)
   4-  5  I2    ---        Seq       ALLSMOG sequential number
   7- 23  A17   ---        Name      Galaxy name
  24- 28  F5.2  [Msun]     logM*     Stellar mass estimated from optical SDSS
                                      observations (1)
  30- 33  F4.2  [Msun]   e_logM*     rms uncertainty on logM*
  35- 39  F5.2 [Msun/yr]   logSFR    Star formation rate estimated from optical
                                      SDSS observations (2)
  41- 44  F4.2 [Msun/yr] e_logSFR    rms uncertainty on logSFR
  46- 49  F4.2  ---        MPA-JHU   ?=- Gas-phase metallicity derived using the
                                      calibration of Tremonti et al.
                                      (2004ApJ...613..898T) (12+log(O/H)) (3)
  51- 54  F4.2  ---        N2PP04    Gas-phase metallicity calculated using the
                                      N2 calibration provided of
                                      Pettini & Pagel (2004MNRAS.348L..59P)
                                      (12+log(O/H)) (3)
  56- 59  F4.2  ---        N2M13     Gas-phase metallicity calculated using the
                                      N2 calibration proposed of Marino et al.
                                      (2013, Cat. J/A+A/559/A114)
                                      (12+log(O/H)) (3)
  61- 64  F4.2  ---        O3N2PP04  Gas-phase metallicity calculated using the
                                      O3N2 calibration of Pettini & Pagel
                                      (2004MNRAS.348L..59P) (12+log(O/H)) (3)
  66- 69  F4.2  ---        O3N2M13   Gas-phase metallicity calculated using the
                                      O3N2 calibration of Marino et al.
                                      (2013, Cat. J/A+A/559/A114)
                                      (12+log(O/H)) (3)
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Note (1): The table lists the median value of the PDF for logM* provided in the
  MPA-JHU catalogue. Its associated error is: 0.5x(P84-P16), where P16 and P84
  are respectively the 16th and the 84th percentile values of the PDF.
Note (2): The value listed in the table is the median value of the PDF for
  logSFR corrected for the SDSS fibre aperture provided in the MPA-JHU
  catalogue, and its associated error is 0.5x(P84-P16).
Note (3): Similar to M* and SFR, the value reported in the table is the median
  of the PDF for 12+log(O/H) provided in the MPA-JHU catalogue and the
  associated error is 0.5x(P84-P16).
  Further information on the quantities listed in this table is provided in
  Sect. 4.
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Byte-by-byte Description of file: tablec5.dat
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   Bytes Format Units    Label     Explanations
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   1-  2  A2    ---      Samp      [A I1 I2] Sample (G1)
   4-  5  I2    ---      Seq       ALLSMOG sequential number
   7- 23  A17   ---      Name      Galaxy name
  24- 25  A2    ---    l_logMHI    [<= ] Limit flag on logMHI
  26- 31  F6.3  [Msun]   logMHI    HI gas mass computed from the integrated HI
                                    21cm emission line flux following Eq. (6)
                                    of the paper
  33- 37  F5.3  [Msun] e_logMHI    ? rms uncertainty on logMHI
  39- 40  A2    ---    l_logMHIc   [<= ] Limit flag on logMHIc
  41- 46  F6.3  [Msun]   logMHIc   HI gas mass corrected for self-absorption as
                                    explained in Sect. 4.2
  48- 52  F5.3  [Msun] e_logMHIc   ? rms uncertainty on logMHIc
  54- 61  A8    ---      Tel       Radio telescope used for the HI 21cm
                                    observations
  63-113  A51   ---      Ref       Reference for the HI 21cm observations used
                                    in this work
     115  A1    ---      Note      [+] Note (1)
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Note (1): For these sources we have re-performed the HI 21cm spectral analysis
  on the original data and used the HI flux (or upper limit on it) measured by
  us to calculate MHI (further details in Sect. 4.2).
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Global notes:
Note (G1): Observations ad follows:
   A  = APEX CO(2-1) observations
   I1 = IRAM CO(1-0) observations
   I2 = IRAM CO(2-1) observations
   I  = IRAM observations
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History:
    From electronic version of the journal

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(End)                                      Patricia Vannier [CDS]    23-Oct-2017