J/A+A/604/A53 ALLSMOG final data release. A new APEX CO survey (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 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:
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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 ?=- 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
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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 3σ-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 2014MNRAS.445.2599B).
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Byte-by-byte Description of file: tablec3.dat
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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)
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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
--------------------------------------------------------------------------------
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 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 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 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
(End) Patricia Vannier [CDS] 23-Oct-2017