J/ApJS/257/43 PHANGS-ALMA: arcsecond CO(2-1) imaging of galaxies (Leroy+, 2021)
PHANGS-ALMA: arcsecond CO(2-1) imaging of nearby star-forming galaxies.
Leroy A.K., Schinnerer E., Hughes A., Rosolowsky E., Pety J., Schruba A.,
Usero A., Blanc G.A., Chevance M., Emsellem E., Faesi C.M., Herrera C.N.,
Liu D., Meidt S.E., Querejeta M., Saito T., Sandstrom K.M., Sun J.,
Williams T.G., Anand G.S., Barnes A.T., Behrens E.A., Belfiore F.,
Benincasa S.M., Beslic I., Bigiel F., Bolatto A.D., den Brok J.S., Cao Y.,
Chandar R., Chastenet J., Chiang I.-D., Congiu E., Dale D.A., Deger S.,
Eibensteiner C., Egorov O.V., Garcia-Rodriguez A., Glover S.C.O., Grasha K.,
Henshaw J.D., Ho I.-T., Kepley A.A., Kim J., Klessen R.S., Kreckel K.,
Koch E.W., Kruijssen J.M.D., Larson K.L., Lee J.C., Lopez L.A., Machado J.,
Mayker N., McElroy R., Murphy E.J., Ostriker E.C., Pan H.-A., Pessa I.,
Puschnig J., Razza A., Sanchez-Blazquez P., Santoro F., Sardone A.,
Scheuermann F., Sliwa K., Sormani M.C., Stuber S.K., Thilker D.A.,
Turner J.A., Utomo D., Watkins E.J., Whitmore B.
<Astrophys. J. Suppl. Ser., 257, 43 (2021)>
=2021ApJS..257...43L 2021ApJS..257...43L
ADC_Keywords: Carbon monoxide; Galaxies, nearby; Millimetric/submm sources;
Interstellar medium; Molecular clouds
Keywords: Interstellar medium ; Giant molecular clouds ; Spiral galaxies ;
Millimeter astronomy ; Galaxy evolution ; CO line emission ;
Barred spiral galaxies ; Disk galaxies ; Galaxies ;
Star formation ; Radio astronomy ; Stellar feedback
Abstract:
We present PHANGS-ALMA, the first survey to map CO J=2-1 line emission
at ∼1" ∼100pc spatial resolution from a representative sample of
90 nearby (d≲20Mpc) galaxies that lie on or near the z=0 "main
sequence" of star-forming galaxies. CO line emission traces the bulk
distribution of molecular gas, which is the cold, star-forming phase
of the interstellar medium. At the resolution achieved by PHANGS-ALMA,
each beam reaches the size of a typical individual giant molecular
cloud, so that these data can be used to measure the demographics,
life cycle, and physical state of molecular clouds across the
population of galaxies where the majority of stars form at z=0. This
paper describes the scientific motivation and background for the
survey, sample selection, global properties of the targets, Atacama
Large Millimeter/submillimeter Array (ALMA) observations, and
characteristics of the delivered data and derived data products. As
the ALMA sample serves as the parent sample for parallel surveys with
MUSE on the Very Large Telescope, the Hubble Space Telescope,
AstroSat, the Very Large Array, and other facilities, we include a
detailed discussion of the sample selection. We detail the estimation
of galaxy mass, size, star formation rate, CO luminosity, and other
properties, compare estimates using different systems and provide
best-estimate integrated measurements for each target. We also report
the design and execution of the ALMA observations, which combine a
Cycle 5 Large Program, a series of smaller programs, and archival
observations. Finally, we present the first 1" resolution atlas of CO
emission from nearby galaxies and describe the properties and contents
of the first PHANGS-ALMA public data release.
Description:
PHANGS-ALMA is a key component of the multiwavelength observational
campaign conducted by the Physics at High Angular resolution in Nearby
Galaxies (PHANGS) project. Combining a Cycle 5 ALMA Large Program
(PI: E. Schinnerer), a suite of smaller programs, and data from the
ALMA archive, PHANGS-ALMA mapped the CO J=2->1 emission, hereafter
CO(2-1), from a cleanly selected sample of 90 of the nearest,
ALMA-accessible, massive, star-forming galaxies.
We used the ALMA main array of 12m dishes in a compact configuration,
which yields ∼1" resolution at Band 6 (ν∼230GHz), corresponding to
∼100 pc linear resolution, or about the size of a massive giant
molecular cloud at the typical distance to our targets. We covered the
area of active star formation in each target using large mosaics that
consisted of ∼100-450 12m pointings per galaxy. Including all pilots
and extensions, observations for PHANGS-ALMA spanned six years, from
early 2013 until the end of 2019. See Section 5.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 83 90 PHANGS-ALMA positions, orientations, and distances
table4.dat 65 90 PHANGS-ALMA physical properties
table11.dat 67 823 PHANGS-ALMA total power observation log
table12.dat 81 479 PHANGS-ALMA 7m observation log
table13.dat 81 184 PHANGS-ALMA 12m observation log
table16.dat 71 90 PHANGS-ALMA cube properties
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See also:
VII/237 : HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)
J/ApJ/551/852 : FCRAO CO survey of the outer Galaxy (Heyer+, 2001)
J/ApJS/149/343 : Giant molecular clouds in M33 (Engargiola+, 2003)
J/AJ/126/1607 : IRAS Revised Bright Galaxy Sample (Sanders+, 2003)
J/AJ/127/2031 : Catalog of neighboring galaxies (Karachentsev+, 2004)
J/ApJ/633/871 : Positions & photometry of HII knots in M51 (Calzetti+, 2005)
J/ApJ/671/333 : Aperture photometry in NGC 5194 (Kennicutt+, 2007)
J/ApJ/654/240 : Giant molecular clouds in M31 (Rosolowsky+, 2007)
J/ApJ/661/830 : Giant molecular clouds of M33 (Rosolowsky+, 2007)
J/ApJ/686/948 : CO in extragalactic giant molecular clouds (Bolatto+, 2008)
J/ApJS/178/56 : CO observations of LMC Giant Molecular clouds (Fukui+, 2008)
J/AJ/136/2782 : Star formation efficiency in nearby galaxies (Leroy+, 2008)
J/ApJS/184/1 : Molecular clouds in the LMC by NANTEN. II. (Kawamura+, 2009)
J/PASP/122/1397 : Spitzer Survey of Stellar Structure in Gal. (Sheth+, 2010)
J/A+A/534/A102 : AMIGA IX. Molecular gas properties (Lisenfeld+, 2011)
J/ApJS/197/16 : CO obs. of LMC molecular clouds (MAGMA). (Wong+, 2011)
J/MNRAS/414/940 : ATLAS3D project. IV. (Young+, 2011)
J/A+A/542/A108 : Giant molecular clouds in M33 (Gratier+, 2012)
J/ApJ/772/107 : Giant molecular clouds in nearby gal. (Donovan Meyer+, 2013)
J/ApJ/777/42 : Kinematic and HI data for the NFGS (Kannappan+, 2013)
J/ApJ/784/3 : PAWS catalogs of GMCs and islands in M51 (Colombo+, 2014)
J/ApJS/219/4 : S4G pipeline 4: multi-component decompositions (Salo+, 2015)
J/ApJ/833/229 : Star forming cloud-giant mol. cloud complexes (Lee+, 2016)
J/AJ/152/50 : Cosmicflows-3 catalog (CF3) (Tully+, 2016)
J/ApJ/831/73 : Galactic MCs with HII regions (Vutisalchavakul+, 2016)
J/ApJ/846/159 : Interferometric CO obs. of CALIFA galaxies (Bolatto+, 2017)
J/A+A/601/A146 : M33 mol. clouds and young stellar clusters (Corbelli+, 2017)
J/MNRAS/465/2471 : Enhanced momentum feedback from clustered SN (Gentry+, 2017)
J/ApJ/843/16 : Galaxy groups within 3500km/s (Kourkchi+, 2017)
J/ApJ/846/71 : M51 ISM structures from the CO maps of PAWS (Leroy+, 2017)
J/ApJ/834/57 : MW molecular clouds from 12CO (Miville-Deschenes+, 2017)
J/ApJ/841/109 : Cloud decomposition & SFR measurements (Ochsendorf+, 2017)
J/ApJS/233/22 : xCOLD GASS catalog (Saintonge+, 2017)
J/ApJ/835/278 : Mol. clouds in the dwarf galaxy NGC6822 (Schruba+, 2017)
J/ApJ/850/207 : Action dynamics of the Local Supercluster (Shaya+, 2017)
J/MNRAS/476/875 : xGASS catalog (Catinella+, 2018)
J/ApJ/857/19 : ALMA view of GMCs in NGC 300 (Faesi+, 2018)
J/ApJ/862/110 : Metallicity measurements in 70 nearby gal. (Schruba+, 2018)
J/ApJ/860/172 : Cloud-scale molecular gas properties in 15 gal. (Sun+, 2018)
J/ApJ/880/127 : EMPIRE: IRAM 30m dense gas survey (Jimenez-Donaire+, 2019)
J/ApJS/244/24 : A z=0 Multiwavelength Galaxy Synthesis. I. (Leroy+, 2019)
J/ApJ/889/5 : HST obs. of Mira variables in NGC1559 (Huang+, 2020)
J/ApJ/897/122 : Rot. velocities for PHANGS sample of galaxies (Lang+, 2020)
J/ApJ/892/148 : Molecular ISM in nearby star-forming galaxies (Sun+, 2020)
J/ApJ/901/L8 : Molecular gas properties of 70 PHANGS-ALMA gal. (Sun+, 2020)
Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Galaxy name
12- 12 A1 --- f_Name X=Galaxy is an extension to the main sample
14- 15 I2 h RAh Hour of Right Ascension (J2000) (1)
17- 18 I2 min RAm Minute of Right Ascension (J2000) (1)
20- 23 F4.1 s RAs Second of Right Ascension (J2000) (1)
25- 25 A1 --- DE- Sign of the Declination (J2000)(1)
26- 27 I2 deg DEd Degree of Declination (J2000) (1)
29- 30 I2 arcmin DEm Arcminute of Declination (J2000) (1)
32- 33 I2 arcsec DEs Arcsecond of Declination (J2000) (1)
35- 40 F6.1 km/s vlsr [-226/2389] Mean velocity relative to LSR (2)
42- 45 F4.1 km/s e_vlsr [1.3/33.1] Uncertainty in vlsr (2)
47- 51 F5.1 deg PA [-14.8/359.1] Orientation, position angle (2)
53- 56 F4.1 deg e_PA [0.1/10] Uncertainty in PA (2)
58- 61 F4.1 deg i [8.9/90] Orientation, inclination (2)
63- 66 F4.1 deg e_i [0.2/43.4] Uncertainty in i (2)
68- 72 F5.2 Mpc Dist [2/23.6] Distance
74- 77 F4.2 Mpc e_Dist [0.09/6] Uncertainty in Dist
79- 83 A5 --- r_Dist References for Dist (3)
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Note (1): Centers from Salo+ (2015, J/ApJS/219/4),
Jarrett+ (2003AJ....125..525J 2003AJ....125..525J), or LEDA (Paturel+ 2003, VII/237;
Makarov+ 2014A&A...570A..13M 2014A&A...570A..13M). See Section 4.1.
Note (2): Orientations and velocities from Lang+ (2020, J/ApJ/897/122)
or Sheth+ (2010, J/PASP/122/1397) or LEDA. See Section 4.1.
Note (3): Distance reference key as follows:
1 = Karachentsev et al. (2004AJ....127.2031K 2004AJ....127.2031K);
2 = Tully et al. (2016AJ....152...50T 2016AJ....152...50T);
3 = Shaya et al. (2017ApJ...850..207S 2017ApJ...850..207S);
4 = Kourkchi et al. (2020AJ....159...67K 2020AJ....159...67K);
5 = Anand et al. (2021MNRAS.501.3621A 2021MNRAS.501.3621A);
6 = Tully et al. (2009AJ....138..323T 2009AJ....138..323T);
7 = Kourkchi & Tully (2017ApJ...843...16K 2017ApJ...843...16K);
8 = Anand et al. (2021MNRAS.501.3621A 2021MNRAS.501.3621A);
9 = Huang et al. (2020ApJ...889....5H 2020ApJ...889....5H);
10 = Leonard et al. (2003ApJ...594..247L 2003ApJ...594..247L);
11 = Freedman et al. (2001ApJ...553...47F 2001ApJ...553...47F);
12 = Barbarino et al. (2015MNRAS.448.2312B 2015MNRAS.448.2312B);
13 = Tonry et al. (2001ApJ...546..681T 2001ApJ...546..681T);
14 = Nugent et al. (2006ApJ...645..841N 2006ApJ...645..841N);
15 = Pierce et al. (1994Natur.371..385P 1994Natur.371..385P);
16 = Ruiz-Lapuente (1996ApJ...465L..83R 1996ApJ...465L..83R)
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Galaxy name
12 A1 --- f_Name X=Galaxy is an extension to the main
sample
14- 18 F5.2 [Msun] logMstar [9.18/11.15] Log of stellar mass
20 A1 --- f_logMstar Source for logMstar (4)
22- 25 F4.1 kpc r25 [3.4/34.2] RC3 25th mag isophotal
B-band radius (5)
27- 29 F3.1 kpc Re [0.9/7.3] Estimated half-mass radius
31- 34 F4.1 kpc lstar [0.7/13.1] Stellar scale length
36- 40 F5.2 [Msun/yr] logSFR [-1.59/1.64] Log of star formation rate
42- 47 A6 --- f_logSFR Source for logSFR (6)
49 A1 --- l_logLCO Upper limit flag for logLCO (7)
51- 54 F4.2 [K.km/s.pc2] logLCO [6.61/9.49]? Log of CO luminosity
56- 59 F4.2 --- Corr [0.97/4.24]? Correction factor
61- 65 F5.2 [Msun] logMHI [7.4/10.31]? Log of HI mass
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Note (4): The near-infrared maps used to estimate stellar mass as follows:
I = IRAC 3.6um data from S4G, Sheth+ (2010, J/PASP/122/1397);
W = WISE1 3.4um maps from Leroy+ (2019, J/ApJS/244/24).
Note (5): RC3 -- de Vaucouleurs+ 1991, VII/155
Note (6): Estimates the star formation rate are from the following:
FUVW4 = a linear combination of GALEX FUV and WISE4 (22um) light;
NUVW4 = a linear combination of GALEX NUV and WISE4 (22um) light;
W4ONLY = uses only WISE4 light.
Note (7): We quote a 5σ upper limit on LCO constructed using a broad
velocity window across the whole map.
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Byte-by-byte Description of file: table11.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Target of the observations
12- 25 A14 --- Project ALMA project code
27- 35 F9.3 d start [57036.9/58823.4] Beginning of observations
in MJD (G1)
37- 45 F9.3 d stop [57036.9/58823.5] End of observations in MJD (G1)
47- 50 F4.1 deg minel [19/83] Minimum elevation during observation
52- 55 F4.1 deg maxel [30/88] Maximum elevation during observation
57- 57 I1 --- Nant [2/4] Number of antennas participating in
the observations
59- 62 F4.2 mm pwv [0/4.4] Precipitable water vapor during the
observation
64- 67 F4.1 Jy/K gain [40.5/48.9]? Jansky per Kelvin calibration
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Byte-by-byte Description of file: table1[23].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Target of the observations
11 A1 --- --- [_]
12 A1 --- m_Name Multiple component on Name ID
14- 26 A13 --- Project ALMA project code
28- 36 F9.3 d start [56316.9/58837.1] Beginning of observations
in MJD (G1)
38- 46 F9.3 d stop [56316.9/58837.2] End of observations in MJD (G1)
48- 51 F4.1 deg minel [19.8/78.8] Minimum elevation during observation
53- 56 F4.1 deg maxel [39/89] Maximum elevation during observation
58- 59 I2 --- Nant [7/51] Number of antennas participating in the
observations
61- 64 F4.2 mm pwv [0.24/4.8] Precipitable water vapor during the
observation
66- 69 F4.1 m minu-v [0/26.7] Minimum baseline
71- 75 F5.1 m medu-v [17/201] Median baseline
77- 81 F5.1 m maxu-v [31.3/710.4] Maximum baseline
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Byte-by-byte Description of file: table16.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Galaxy name
12- 20 A9 --- Arrays Best available array combination
22- 25 F4.2 arcsec Res1 [0.6/8.7] Angular resolution of native cube
27- 31 F5.1 pc Res2 [26.2/588.6] Physical resolution
33- 36 F4.1 arcsec2 Area1 [0.7/98.7] Angular area mapped
38- 42 F5.1 kpc2 Area2 [8.1/396.8] Physical area mapped
44- 46 I3 mK Noise1 [18/366] Noise in surface brightness,
Native resolution in mK
48- 50 I3 mK Noise2 [13/114]? Noise in surface brightness, 150pc
52- 56 F5.1 mJy/beam Noise3 [1.3/128.1] Noise in surface brightness,
Native resolution in mJy/beam
58- 61 F4.1 % Comp1 [1.7/97] Completeness, Native resolution (8)
63- 63 A1 --- f_Comp1 F=Faint galaxy, completeness is unreliable
65- 69 F5.1 % Comp2 [0.9/180]? Completeness, 150pc (8)
71 A1 --- f_Comp2 F=Faint galaxy, completeness is unreliable
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Note (8): Completeness defined as the ratio of flux inside the strict mask
to the sum of the cube or the broad mask.
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Global notes:
Note (G1): Modified Julian Day (00:00 on Jan 1, 2018 is MJD 58119)
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 03-Mar-2022