J/A+A/327/522 Molecular gas content of spiral galaxies (Boselli+ 1997)
The molecular gas content of spiral galaxies in the Coma/A1367 supercluster Boselli A., Gavazzi G., Lequeux J., Buat V., Casoli F., Dickey J., Donas J. <Astron. Astrophys. 327, 522 (1997)> =1997A&A...327..522B
ADC_Keywords: Galaxies, spectra - Radio lines Keywords: Galaxies: general - spiral - ISM - intergalactic medium - star formation - radio lines: galaxies Description: We present 12CO(J=1-0) line observations of 73 spiral galaxies mostly in the Coma/A1367 supercluster. From these data, combined with data available in the literature, we extract the first complete, optically selected sample (mpg<15.2) of 37 isolated and of 27 cluster galaxies. The 12CO(1-0) line spectra are accessible as postscript figures. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 89 73 Target galaxies table2.dat 59 73 Results of CO observations table3.dat 109 72 Parameters of the optically selected galaxies fig/* 0 71 12CO(1-0) line spectra
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 7 A7 --- CGCG CGCG designation (1) 10- 13 I4 --- NGC/IC ? NGC/IC number 16- 20 I5 --- UGC ? Designation in UGC VII/26 22- 23 I2 h RAh Right Ascension B1950 (hours) (2) 24- 25 I2 min RAm Right Ascension B1950 (minutes) (2) 26- 30 F5.2 s RAs Right Ascension B1950 (seconds) (2) 32 A1 --- DE- Declination B1950 (sign) (2) 33- 34 I2 deg DEd Declination B1950 (degrees) (2) 35- 36 I2 arcmin DEm Declination B1950 (minutes) (2) 37- 40 F4.1 arcsec DEs Declination B1950 (seconds) (2) 43- 45 A3 --- MType Morphological type from Gavazzi+Boselli (1996) 50- 52 A3 --- Agg Aggregation (membership) note (3) 56- 60 I5 km/s RVel Heliocentric velocity, from Gavazzi (1989ApJ...346...59G) and references therein. 62- 66 F5.1 Mpc Distance Distance determined using Ho = 100km/s/Mpc (4) 68- 72 F5.2 arcmin MajDiam Galaxy major diameter (5) 74- 78 F5.2 arcmin MinDiam Galaxy minor diameter (5) 81- 84 F4.1 mag Pmag Photographic magnitude as given in the CGCG. 86- 89 I4 km/s HIwidth ? Width of the HI line (6)
Note (1): The first 3 digits indicate the field number, the last 3 the source number in the field; see catalog VII/49. Note (2): Celestial coordinates with a few arcsec accuracy, from Gavazzi & Boselli (1996), Astrophys. Letters and Comm. 35, 1 Note (3): The Aggregation note has the following values: A = member of A1367 C = member of Coma cluster I = isolated; G = group; P = pair; N = NGC 5056 group I, G, P and N are all included in the Coma supercluster region (see Gavazzi, 1987ApJ...320...96G for more details) H51 and H97 = member of A2151 and A2197 in the Hercules supercluster, cA and cD = member of the cloud A and D in the Cancer cluster (Bothun et al. 1984AJ.....89.1300B). Note (4): we assume 69 Mpc for the Coma cluster and 65 Mpc for A1367 as in Gavazzi (1987ApJ...320...96G) For galaxies belonging to groups, the distances are determined from their average redshifts. For double systems or isolated supercluster objects, distances are determined from the individual redshifts. Cloud A Cancer galaxies are taken at 47 Mpc, cloud D at 36 Mpc. Galaxies in the Hercules supercluster are assumed at 110 Mpc (A2151), and at 92 Mpc (A2197). Note (5): Galaxy major and minor optical blue diameters, in arcminutes, from Gavazzi & Boselli (1996). These are isophotal diameters at the 25th mag/arcsec2 determined from available CCDs. Note (6): Width of the HI line averaged between 20 and 50 % of its maximum, from Gavazzi (1989ApJ...346...59G) and references therein.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 7 A7 --- CGCG CGCG designation, as in table1.dat 10- 12 I3 min Itime Integration time (on+off) 14- 17 F4.2 mK rms rms noise, in mK, in the T*R scale. 20 A1 --- l_I(CO) Limit flag on I(CO) 21- 24 F4.2 K.km/s I(CO) Intensity of the I(CO) line (1) 27- 30 F4.2 K.km/s e_I(CO) Error on CO intensity I(CO) (2) 33- 37 I5 km/s V(CO) ? Heliocentric velocity from the CO line (3) 40- 42 I3 km/s DV(CO) ? Width at 50% of the CO line 44 A1 --- l_logMiH2 Limit flag on logMiH2 45- 48 F4.2 [solMass] logMiH2 "Indicative" H2 mass (see Sect. 4.1) 50- 59 A10 --- File File name (in subdirectory fig) (4)
Note (1): For undetected galaxies, the reported value is an upper limit determined as: I(CO) = 2σ (ΔV(HI).δV(CO))1/2 where σ is the rms noise of the spectrum, ΔV(HI) is the HI line width δV(CO) is the spectral resolution (20km/s) For galaxies with ΔV(HI) not available, the HI width has been determined assuming a standard ΔV(HI) = 300 sin(i) km/s, where i is the galaxy inclination, or ΔV(HI) = 50 km/s if i = 0. Note (2): The error e_I(CO) is computed as e_I(CO) = 2σ (ΔV(CO).δV(CO))1/2 where σ is the rms noise of the spectrum, ΔV(CO) is the CO linewidth (given in Col. 7), and δV(CO) is the spectral resolution. Spectra were smoothed to δV(CO) = 20 km/s Note (3): Heliocentric velocity determined with a gaussian fit (optical definition v=cz=Δλ/λ0). The estimated error is comparable with the resolution, thus 20 km/s Note (4): two figures are missing because the FITS files were corrupted.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 7 A7 --- CGCG CGCG designation (1) 9- 11 A3 --- MType Morphological type from Gavazzi+Boselli (1996) 16 A1 --- Agg [ACGIP] Membership note (2) 19- 22 F4.2 --- W05 [0/1] Cluster membership assigned (3) 24- 28 F5.2 arcmin MajDiam Galaxy major diameter as in table1.dat 30- 34 F5.2 arcmin MinDiam Galaxy minor diameter as in table1.dat 36- 40 F5.1 Mpc Distance determined using H0 = 100 km/s/Mpc 43- 47 F5.2 mag Hc Corrected H magnitude from Gavazzi+Boselli (1996) 50- 54 F5.2 mag Bc Corrected B magnitude from Gavazzi+Boselli (1996) 57- 61 F5.2 mag UV ? Uncorrected UV 200nm magnitude (4) 63 A1 --- l_M(HI) Limit flag on M(HI) 64- 68 F5.2 [solMass] M(HI) ? logarithm of the atomic hydrogen mass, as in Gavazzi (1987ApJ...320...96G) 70 A1 --- l_HIdef Limit flag on HIdef 71- 75 F5.2 --- HIdef ? HI deficiency, determined as in Haynes and Giovanelli (1984AJ.....89..758H) 78 A1 --- l_MiH2 Limit flag on MiH2 79- 83 F5.2 [solMass] MiH2 Logarithm of the indicative molecular hydrogen content, as described in section 4.1. 86 I1 --- Ref References to the CO data (5) 88- 91 F4.2 --- r ? Ratio of optical diameter to HPBW (6) 92 A1 --- n_r [*m] Note on r (6) 95- 96 I2 0.1nm Halpha ? Halpha equivalent width from Gavazzi et al. (1991AJ....101.1207G) + references therein. 97 A1 --- n_Halpha [*] Recently observed galaxy (7) 98-102 F5.2 mag U-B ? (U-B)c Corrected colour from Gavazzi+Boselli (1996) 105 A1 --- l_FIR/H Limit flag on FIR/H 106-109 F4.2 [---] FIR/H ? Far IR to U ratio in logarithmic scale (8)
Note (1): The first 3 digits indicate the field number, the last 3 the source number in the field; see catalog VII/49. Note (2): as in Table 1, the Aggregation note has the following values: A = member of A1367; C = member of Coma cluster; I = isolated; G = group; P = pair; N = NGC 5056 group Note (3): Cluster membership assigned according to the statistical method described in Gavazzi et al. (1995ApJ...438..590G), based on dynamical considerations (hereafter referred as the "caustic" criterium). If W is the weighting function defined in Gavazzi et al. 1995 for Ωo = 0.5, indicating the probability to a galaxy to reside within the caustic (thus the probability to be dynamically related to the cluster), we assume cluster members those objects with W > 0.80 and isolated galaxies those with W < 0.80. As discussed in Gavazzi et al., the "caustic" criterium is less restrictive than the "aggregation" criterium since it includes in the cluster sample some objects at larger angular distances. Note (4): From Donas et al. (1990A&A...235...60D; 1995A&A...303..661D) Note (5): References are numbered as follows: 1 = this work, 1994 run; 2 = this work, 1995 run; 3 = this work, 1996 run; 4 = Boselli et al. (1994A&A...285...69B); 5 = Boselli et al. (1995A&AS..110..521B); 6 = Casoli et al. (1991A&A...249..359C); 7 = Dickey & Kazes (1992ApJ...393..530D); 8 = Casoli et al. (1996A&AS..116..193C) Note (6): ratio r of the optical diameter to the HPBW of the telescope used in the CO observations. The note indicates: m indicates mapped objects; galaxies marked * indicates the galaxies observed also with the 12m Kitt Peak telescope (HPBW = 55"; see Casoli et al. 1996A&AS..116..193C), with consistent results. r gives a raw estimate of the CO sampling of the target galaxy. Given the peaked CO distribution compared with the optical one (see Sect. 4.1), the observations should give accurate measurement of the total CO emission of galaxies with r<2, while they should underestimate by a factor of <2 the total CO emission of objects with r=4 (Sauty et al., in preparation). Note (7): An * indicates galaxies recently observed, for which only preliminary data (used in the following analysis) are available; these Hα data will be presented in a forecoming paper (Gavazzi et al., in preparation). Note (8): the ratio FIR/H, in logarithmic scale, determined from the 60um FIR flux (in mJy) and the Hflux (in mJy), defined as Hflux = 1.030x106 . 10-Hc/2.5 mJy.
Acknowledgements: Alessandro Boselli References: Gavazzi, G., and Boselli. A., 1996, Astrophys. Letters and Comm. 35, 1
(End) Patricia Bauer [CDS] 09-Jun-1997
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