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J/A+A/420/97        Tully-Fisher relation at 0.1<z<1.0         (Boehm+, 2004)

The Tully-Fisher relation at intermediate redshift. Boehm A., Ziegler B.L., Saglia R.P., Bender R., Fricke K.J., Gabasch A., Heidt J., Mehlert D., Noll S., Seitz S. <Astron. Astrophys. 420, 97 (2004)> =2004A&A...420...97B
ADC_Keywords: Galaxies, photometry ; Rotational velocities ; Redshifts Keywords: galaxies: spiral - galaxies: evolution - galaxies: kinematics and dynamics Abstract: Using the Very Large Telescope in Multi Object Spectroscopy mode, we have observed a sample of 113 field spiral galaxies in the FORS Deep Field (FDF) with redshifts in the range 0.1<z<1.0. The galaxies were selected based on apparent brightness (R<23) and encompass all late spectrophotometric types from Sa to Sdm/Im. Spatially resolved rotation curves have been extracted for 77 galaxies and fitted with synthetic velocity fields taking into account all observational effects from inclination and slit misalignment to seeing and slit width. We also compared different shapes for the intrinsic rotation curve. To obtain robust values of Vmax, our analysis is focused on galaxies with rotation curves that extend well into the region of constant rotation velocity at large radii. If the slope of the local Tully-Fisher relation (TFR) is held fixed, we find evidence for a mass-dependent luminosity evolution which is as large as up to 2mag for the lowest-mass galaxies, but is small or even negligible for the highest-mass systems in our sample. In effect, the TFR slope is shallower at z∼0.5 in comparison to the local sample. We argue for a mass-dependent evolution of the mass-to-light ratio. An additional population of blue, low-mass spirals does not seem a very appealing explanation. The flatter tilt we find for the distant TFR is in contradiction to the predictions of recent semi-analytic simulations. Description: Structural parameters, redshifts, spectral types, luminosities and maximum rotation velocities are presented for a sample of 77 spiral galaxies in the FORS Deep Field. The galaxies cover the redshift range 0.1<z<1.0 and comprise all spectrophotometric types from Sa to Sdm/Im. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 80 77 Photometric and kinematic data on 77 spirals in the FORS Deep Field
See also: J/A+A/398/49 : UBgRIJKs photometry in the FORS Deep Field (Heidt+, 2003) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 4 I4 --- FDF FORS Deep Field photometric catalogue number (as in Cat. J/A+A/398/49) 6- 7 I2 deg i Disk inclination angle (0 = face-on) 9- 10 I2 deg delta Misalignment angle between disk major axis and slitlet 12- 15 F4.2 arcsec rd Exponential disk scale length (1) 17- 22 F6.4 --- z Spectroscopic redshift 24- 25 I2 --- TType SED classifier in the de Vaucouleurs scheme 27- 31 F5.2 mag Xmag Total apparent magnitude in filter X (2) 33- 37 F5.2 mag kB K-correction (to rest-frame Johnson B) 39- 42 F4.2 mag AX Galactic absorption (in filter X) 44- 47 F4.2 mag AB Intrinsic absorption in rest-frame B (3) 49- 53 F5.2 mag m-M Distance modulus (4) 55- 60 F6.2 mag BMAG B-band absolute magnitude 62- 65 F4.2 mag e_BMAG Error on B-band absolute magnitude 67- 69 I3 km/s Vmax Intrinsic maximum rotation velocity (5) 71- 73 I3 km/s e_Vmax Error on intrinsic maximum rotation velocity 75- 78 F4.2 mag B-R Rest-frame extinction-corrected B-R color index 80 A1 --- Qual Rotation curve quality (6)
Note (1): Structural parameters were derived from 2-D surface brightness profile fitting on ground-based images taking into account the seeing. According to our simulations, the disk scale length is not a crucial input parameter for the determination of Vmax in the case of distant spirals. However, some values of rd may be affected by the limitations of the ground-based imaging. We therefore recommend not to use these scale lengths for applications like the Fundamental Plane of spiral galaxies. Note (2): Apparent magnitude is given for the filter X which best matches the rest-frame B-band. For objects with z<0.25, this is the B-band, in the range 0.25<z<0.55 the g-band was used, for 0.55<z<0.85, the R-band was used, and at z>0.85 the I-band. Note (3): Intrinsic absorption is computed following Tully & Fouque (1985ApJS...58...67T). Note (4): Adopting the concordance cosmology with Ωλ=0.7, Ωm=0.3 and H0=70km/s/Mpc. Note (5): Derived via synthetic velocity fields assuming a linear rise of the rotation velocity at small galactocentric radii and a flat rotation curve at large radii ("rise-turnover-flat" shape). Note (6): Quality flags: "H" - High quality, symmetric rotation curves with a clearly visible flat part at large radii. These objects are usable for Tully-Fisher applications. "L" - Low quality rotation curves with relatively small spatial extent and/or asymmetric shapes.
Acknowledgements: Asmus Boehm
(End) Asmus Boehm [University Observatory Goettingen, Germany] 25-Mar-2004
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

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