Access to Astronomical Catalogues

← Click to display the menu
J/A+A/604/A53           Final data release of ALLSMOG            (Cicone+, 2017)

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)
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 (108.5<M*[M]<1010) 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*<109M 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 (AV), 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*=108.5M to M*=1011M. 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 AV<0.5mag may reveal an as much steep correlation with AV. 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 MHI. 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, νCO(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, νCO(1-0)=115.271GHz) and CO(2-1) emission lines in a sample of nine additional galaxies characterised by stellar masses, M*<109M. A total of 22h of observations were obtained with the IRAM 30m during two observing runs in November 2014 and May 2015. File Summary:
FileName Lrecl Records Explanations
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
Byte-by-byte Description of file: tablec1.dat
Bytes Format Units Label Explanations
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 ?=- 1σ spectral rms calculated in channels of δv=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 3σ 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
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 3σ-upper limit on the total integrated CO flux derived using Eq. (3).
Byte-by-byte Description of file: tablec2.dat
Bytes Format Units Label Explanations
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
Note (1): calculated as explained in Sect. 3.5 following the same method as Bothwell et al. (2014MNRAS.445.2599B).
Byte-by-byte Description of file: tablec3.dat
Bytes Format Units Label Explanations
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)
Note (1): Further details are given in Sect. 4.1 Note (2): Both i and d25 are drawn from the Hyperleda database.
Byte-by-byte Description of file: tablec4.dat
Bytes Format Units Label Explanations
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)
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.
Byte-by-byte Description of file: tablec5.dat
Bytes Format Units Label Explanations
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)
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).
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
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 23-Oct-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© UDS/CNRS

Contact