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J/A+A/370/765       HI synthesis observations in UMa cluster (Verheijen+, 2001)

The Ursa Major cluster of galaxies. IV. HI synthesis observations. Verheijen M.A.W., Sancisi R. <Astron. Astrophys. 370, 765 (2001)> =2001A&A...370..765V
ADC_Keywords: Clusters, galaxy ; H I data ; Galaxies, rotation ; Photometry Keywords: galaxies: fundamental parameters - galaxies: kinematics and dynamics - galaxies: spiral - galaxies: structure Abstract: In this data paper we present the results of an extensive 21 cm-line synthesis imaging survey of 43 spiral galaxies in the nearby Ursa Major cluster using the Westerbork Synthesis Radio Telescope. Detailed kinematic information in the form of position-velocity diagrams and rotation curves is presented in an atlas together with HI channel maps, 21 cm continuum maps, global HI profiles, radial HI surface density profiles, integrated HI column density maps, and HI velocity fields. The relation between the corrected global HI linewidth and the rotational velocities Vmax and Vflat as derived from the rotation curves is investigated. Inclination angles obtained from the optical axis ratios are compared to those derived from the inclined HI disks and the HI velocity fields. The galaxies were not selected on the basis of their HI content but solely on the basis of their cluster membership and inclination which should be suitable for a kinematic analysis. The observed galaxies provide a well-defined, volume limited and equidistant sample, useful to investigate in detail the statistical properties of the Tully-Fisher relation and the dark matter halos around them. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 86 52 All galaxies in the UMa cluster brighter than Mb,i(B)=-16.8 and more inclined than 45 degrees table2.dat 92 52 Photometry of all galaxies in the UMa cluster brighter than Mb,i(B)=-16.8 and more inclined than 45 degrees table3.dat 68 57 A comparison of the widths and integrated fluxes from the present WSRT survey and from the literature table4.dat 48 437 Rotation curves derived from velocity fields and XV-diagrams table5.dat 104 43 Results from the HI synthesis observations literature
See also: J/AJ/112/2471 : The Ursa Major cluster. I. (Tully+ 1996) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 2 A2 --- Sample Samples (G1) 4- 10 A7 --- Name Galaxy name (U for UGC, N for NGC) 11 A1 --- n_Name [fi] Note on the galaxy (2) 13- 14 I2 h RAh Right ascension (B1950) 16- 17 I2 min RAm Right ascension (B1950) 19- 22 F4.1 s RAs Right ascension (B1950) 24 A1 --- DE- Declination sign (B1950) 25- 26 I2 deg DEd Declination (B1950) 28- 29 I2 arcmin DEm Declination (B1950) 31- 32 I2 arcsec DEs Declination (B1950) 34- 39 F6.2 deg GLON Galactic longitude 41- 45 F5.2 deg GLAT Galactic latitude 47- 50 A4 --- MType Morphological type 52- 55 F4.2 arcmin D25(B) Observed major axis diameter of the 25th mag/arcsec2 blue isophote 57- 59 I3 deg PA Position angle of the receding side of the galaxy (3) 61- 64 F4.2 --- 1-b/a Observed ellipticity of the optical galaxy image 66- 67 I2 deg iopt Inclination as derived from the observed axis ratio (b/a). 69- 70 I2 deg iadopt Adopted inclination angle as derived from several methods 72 I1 deg e_iadopt rms uncertainty on iadopt 74- 76 A3 --- SB Low (LSB) or high surface brightness (HSB) galaxy, according to Paper II 78- 81 F4.2 mag [BH] Galactic extinction in the B-band according to Burstein & Heiles (1984ApJS...54...33B) 83- 86 F4.2 mag [SFD] Galactic extinction in the B-band according to Schlegel et al. (1998ApJ...500..525S)
Note (2): There are 3 additional galaxies in the tables which do not meet the luminosity (f) and inclination (i) criteria but happened to be in the same WSRT fields as galaxies from the complete sample. Note (3): For galaxies which are not observed or not detected in HI, this is the smallest position angle of the major axis measured eastward from the north.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 2 A2 --- Sample Samples (G1) 4- 10 A7 --- Name Galaxy name (U for UGC, N for NGC) 11 A1 --- n_Name [fi] Note on the galaxy (2) 13- 17 F5.2 mag Bmag Total B magnitude (3) 19- 23 F5.2 mag Rmag Total R magnitude (3) 25- 29 F5.2 mag Imag Total I magnitude (3) 31- 35 F5.2 mag K'mag ? Total K'mag magnitude (3) 37- 39 I3 km/s WHI ? Corrected HI line width at the 20% level, used to calculate the internal extinction 41- 44 F4.2 mag AB Calculated internal extinction corrections in the B passband (4) 46- 49 F4.2 mag AR Calculated internal extinction corrections in the R passband (4) 51- 54 F4.2 mag AI Calculated internal extinction corrections in the I passband (4) 56- 59 F4.2 mag AK' Calculated internal extinction corrections in the K' passband (4) 61- 66 F6.2 mag BMAG Ttal absolute B magnitude (5) 68- 73 F6.2 mag RMAG Total absolute R magnitude (5) 75- 80 F6.2 mag IMAG Total absolute I magnitude (5) 82- 87 F6.2 mag K'MAG ? Total absolute K' magnitude (5) 89- 92 F4.2 arcmin D25 Diameter of the 25th mag/arcsec^2^ blue isophote (6)
Note (2): There are 3 additional galaxies in the tables which do not meet the luminosity (f) and inclination (i) criteria but happened to be in the same WSRT fields as galaxies from the complete sample. Note (3): Total magnitudes form paper I (Tully et al., 1996AJ....112.2471T) Note (4): Calculated internal extinction corrections toward face-on Ai->0lambda according to Tully et al. (1998AJ....115.2264T): Ai->0lambda = γλ*log(a/b) where a/b is the observed axis ratio of the galaxy as an indication of inclination while γλ depends on the luminosity and is calculated according to: γB = 1.57 + 2.75(logWiR,I - 2.5) γR = 1.15 + 1.88(logWiR,I - 2.5) γI = 0.92 + 1.63(logWiR,I - 2.5) γK'= 0.22 + 0.40(logWiR,I - 2.5) where WiR,I is the distance independent HI line width corrected for instrumental resolution, corrected for turbulent motion according to Tully & Fouqui (1985ApJS...58...67T) (TFq hereafter) with Wt,20=22km/s as motivated in Sect. 4 and corrected for inclination using iadopt from table1. Note (5): Total absolute magnitudes corrected for Galactic and internal extinction and a distance modulus of 31.35 corresponding to a distance to the Ursa Major cluster of 18.6 Mpc Note (6): Diameter corrected for both galactic and internal extinction and projection
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 5 A5 --- Name Galaxy name (U for UGC, N for NGC) 6- 10 A5 --- n_Name Note on Name (1) 12- 16 F5.1 km/s W20 HI line width at the 20% level, this work 18- 20 F3.1 km/s e_W20 rms uncertainty on W20 22- 25 F4.1 km/s Res Velocity resolution, this work 27- 31 F5.1 Jy.km/s Int Integrated flux, this work 33- 35 F3.1 Jy.km/s e_Int rms uncertainty on Int 37- 39 I3 km/s W20l ? HI line width at the 20% level, from Ref 40 A1 --- n_W20l [m?] Note on W20l (1) 42- 43 I2 km/s e_W20l ? rms uncertainty on W20l 45- 48 F4.1 km/s Resl ? Velocity resolution, from Ref 50- 54 F5.1 Jy.km/s Intl ? Integrated flux, from Ref 55 A1 --- n_Intl [?!] Note on Intl (1) 57- 60 F4.1 Jy.km/s e_Intl ? rms uncertainty on Intl 62- 63 I2 --- r_Intl ? References (2) 65- 68 A4 --- Obs Synthesis observation with the WRST or the VLA
Note (1): Notes: (c): the authors suggest possible confusion with a dwarf companion. c: flagged by the authors as confused with near companion. l: large correction factor (>1.20) applied for primary beam flux attenuation. i: flagged by the authors as possibly interacting. noSD: no useful single dish profile available due to obvious confusion. m: line width directly measured from the published HI profile. !: the integrated flux as quoted by the author is a factor 2 larger than is quoted by any other source. Therefore, half the integrated flux was adopted from this source. Note (2): References: 1: Fisher & Tully (1981ApJS...47..139F) 2: Appleton & Davies (1982MNRAS.201.1073A) 3: Richter & Huchtmeier (1991A&AS...87..425R) 4: Oosterloo & Shostak (1993A&AS...99..379O) 5: Huchtmeier & Richter (1986A&AS...63..323H) 6: Schneider et al. (1992ApJS...81....5S) 7: Jore et al. (1996AJ....112..438J) 8: Schwarz (1985A&A...142..273S) 9: Thuan & Martin (1981ApJ...247..823T) 10: Magri (1994AJ....108..896M) 11: Van der Burg (1987, Ph.D. Thesis, University of Groningen) 12: Gottesman et al. (1984ApJ...286..471G) 13: Van Moorsel (1983A&AS...54....1V) 14: Grewing & Mebold (1975A&A....42..119G)
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 2 A2 --- Sample [F X] Sample (1) 4- 8 A5 --- Name Galaxy name (N for NGC, U for UGC) 10- 12 I3 arcsec Rad Radius 14- 16 I3 km/s VrotApp ? Approaching rotation velocity 18- 20 I3 km/s VrotAppM ? Maximum value of approaching rotation velocity 22- 24 I3 km/s VrotAppm ? Minimum value of approaching rotation velocity 26- 28 I3 km/s VrotRec ? Receding rotation velocity 30- 32 I3 km/s VrotRecM ? Maximum value of receding rotation velocity 34- 36 I3 km/s VrotRecm ? Minimum value of receding rotation velocity 38- 40 I3 km/s Vrot ? Average rotational velocity 42- 44 I3 deg Incl Inclination 46- 48 I3 deg PA [13/381] Position angle
Note (1): Samples: FX: Rotation curves derived from velocity fields and XV-diagrams X: Rotation curves derived from XV-diagrams only
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 2 A2 --- Sample [FPH] Sample (G1) 4- 8 A5 --- Name Galaxy name (N for NGC, U for UGC) 10- 14 F5.1 km/s W20 Uncorrected widths with formal errors of the global profiles at 20% of the peak flux 16- 18 F3.1 km/s e_W20 rms uncertainty on W20 20- 24 F5.1 km/s W50 Uncorrected widths with formal errors of the global profiles at 50% of the peak flux 26- 28 F3.1 km/s e_W50 rms uncertainty on W50 30- 33 F4.1 km/s Res Instrumental velocity resolution at which the global profiles were observed 35- 40 F6.1 km/s HRV Heliocentric systemic velocity as derived from the global profiles 42- 44 F3.1 km/s e_HRV rms uncertainty on HRV 46- 50 F5.1 Jy.km/s Int Integrated HI flux 52- 54 F3.1 Jy.km/s e_Int rms uncertainty on Int 56 A1 --- l_F21cm Limit flag on F21cm 57- 61 F5.1 mJy F21cm 21cm (1400MHz) continuum flux density (2) 63- 65 F3.1 mJy e_F21cm ? rms uncertainty on F21cm 67- 70 F4.2 arcmin RHI ? Radius of the HI disk (3) 72- 75 F4.2 arcmin Rlmp ? Radius of the last measured point of the rotation curve (4) 77- 79 I3 km/s Vlmp ? Rotational velocity of the last measured point 81- 82 I2 km/s e_Vlmp ? rms uncertainty on Vrot 84- 90 A7 --- Shape Information on the overall shape of the rotation curve (5) 92- 94 I3 km/s Vmax ? Maximum observed rotational velocity (6) 96- 97 I2 km/s e_Vmax ? rms uncertainty on Vmax 99-101 I3 km/s Vflat ? Average rotational velocity of the flat part of the rotation curve (7) 103-104 I2 km/s e_Vflat ? rms uncertainty on Vflat
Note (2): In case no continuum flux was detected, a 3σ upper limit for extended emission is given. Note (3): Radius at the azimuthally averaged surface density of 1M_☉/pc2, measured from the radial surface density profiles. Note (4): The differences between Rlmp and RHI depend on the sensitivity of the measurement and the distribution of the HI gas along the kinematic major axis. Note (5): Overal shape of the rotation curve: R: rising rotation curve F: the rotation curve shows a flat part D: the rotation curve shows a declining part L: lopsided Note (6): For galaxies with a rising rotation curve (R) Vmax=Vlmp Note (7): For galaxies with a flat rotation curve (F) Vflat=Vmax may deviate from Vlmp because V_flat was averaged over the flat part of the rotation curve while Vlmp was measured at a single point.
Global Notes: Note (G1): the sample values are: FH: Galaxies with fully analyzed HI data PH: Galaxies with partially analyzed HI data CH: Galaxies with confused HI data NH: Not observed or too little HI content
History: From electronic version of the journal References: Tully et al., Paper I 1996AJ....112.2471T, Cat. J/AJ/112/2471 Tully & Verheijen, Paper II 1997ApJ...484..145T
(End) Patricia Bauer [CDS] 05-Jun-2001
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