|
goldmine glossary |
|
General references Specific references to GOLDMine data |
||
|
CGCG
UV Magnitude Total 2000 A magnitude as given in: Donas J., Milliard B., Laget M., Buat V., 1990, A&A, 235, 60 Donas J., Milliard B., Laget M., 1995, A&A, 303, 661 Deharveng J.M., Sasseen T., Buat V., Bowyer S., Lampton M., Wu X., 19 94, A\&A, 289, 715 (FAUST) or given us by J. Donas (private communication). These are total (not aperture) UV magnitudes extracted from the photographic plates. Data taken with the FAUST experiment at 1650 AA were converted to 2000 AA using: UV_(2000)=UV_(1650)+0.2 mag. The quoted error on the UV magnitude is 0.3 mag in general, but it ranges from 0.2 mag for bright galaxies to 0.5 mag for weak sources observed in frames with larger than average calibration uncertainties. Optical (U,B,V) Magnitudes Total magnitudes (U,B,V) computed at the optical radius (25th magnitude / arcsec^2). The assumed photometrical uncertainties are 15% for B, V and 20% for U. Optical magnitudes derive from published aperture/ccd photometry or from several imaging campaigns carried out with the Loiano 1.5m and San Pedro Martir 2.1m telescopes. See: Astrophysical Letters & communcations 1996 vol. 35 p. 1 Gavazzi, G., Boselli, A. A UBVJHK Photometric catalogue of 1022 galaxies in 8 nearby clusters NIR (J,H,K) Magnitudes Total Near Infrared magnitudes (J,H,K) computed at the optical radius (25th magnitude / arcsec^2). The assumed photometrical uncertainties are 15% for H and 20% for J and K. NIR magnitudes derive from data taken during observational campaigns carried out with infrared telescopes (TIRGO 1.5m, Calar Alto 2.2m, 3.5m, TNG 3.6m, ESO/NTT). See: Astrophysical Letters & communcations 1996 vol. 35 p. 1 Gavazzi, G., Boselli, A. A UBVJHK Photometric catalogue of 1022 galaxies in 8 nearby clusters IRAS data IRAS 60 and 100 micron fluxes (in Jy) with sign ("."=detected; "<"=upper limit). RADIO data Radio Continuum fluxes (in mJy) at 21 and 50 cm (1420 and 610 MHz) with sign ("."=detected; "<"=upper limit). The 1420 MHz flux is generally derived from the NVSS survey of Condon et al. (1998). The 610 MHz flux is from Gavazzi (1979) and Jaffe et al. (1986). See: 1999A&A...343...93G On the local radio luminosity function of galaxies. II. Environmental dependences among late-type galaxies. GAVAZZI G., BOSELLI A. 1999A&A...343...86G On the local radio luminosity function of galaxies. I. The Virgo cluster. GAVAZZI G., BOSELLI A. Note: For Virgo galaxies the 50 cm Flux is derived from the 2380 MHz Flux of Dressel & Condon: 1978, Ap.J.Suppl.,36,53 converted to 610 using a spectral index 0.80. Line photometry parameters HI Mass Neutral Hydrogen mass (Log solar masses) with sign ("."=detected; "<"=upper limit) obtained using: MHI=2.36*(10.**5)*(dist**2)*SHI where SHI is the flux in the HI line (in mJy km/sec) and dist is the distance in Mpc. Our data derive from observational campaigns carried out in the 21cm line using the Arecibo telescope, with VLA and with the Nancay radio telescope. H_2 Mass Molecular Hydrogen mass (Log solar masses) with sign ("."=detected; "<"=upper limit) obtained with a luminosity dependent C conversion factor, as explained in: Boselli, A.; Lequeux, J.; Gavazzi, G. Astronomy and Astrophysics, v.384, p.33-47 (2002) Molecular gas in normal late-type galaxies. Data derive from several observational campaigns carried out with millimetric radio telescopes (IRAM, SEST, ONSALA, KPNO) (Boselli et al. 1994, 1995a,b, 1997b, 2002b; Casoli et al. 1996a,b, 1998). H_alpha Equivalent Width Equivalent width of the H_alpha[+NII] line (in AA). The census of currently forming (younger than 10^7 yrs) massive (M>5 Msol) stars is best achieved by observing the Balmer recombination line H_alpha (6563 AA in the red visible domain) which is emitted by the ionized gas surrounding the regions of current star formation (HII regions). Our data derive from several observational campaigns of H_alpha line emission imaging carried out with optical telescopes (KPNO 1.3m, SPM 2.1m, OHP 1.2m, INT 2.5m, NOT 2.5m, Calar Alto 1.2m) by Gavazzi et al. (1991, 1998, 2000a, 2001a, 2002a,b); Boselli et al. (2002c,d); Iglesias Paramo et al. (2002). H_alpha Flux Log of Flux in the H_alpha[+NII] line (in erg/ cm^2 s) (same references as above). Dynamical parameters Width of HI line Observed width of the HI line (in km/sec) obtained by averaging the value at 20% of the peak flux with the one at 50% of the mean flux. See Scodeggio and Gavazzi, 1993, ApJ, 409, 110 21 centimeter study of spiral galaxies in clusters. III Neutral gas content, star formation, and radio continuum properties. HI Quality Quality of the HI spectrum. 1= good quality, high signal-to-noise, double-horned spectra 2= good quality, high signal-to-noise, single-horned spectra 3= medium quality, medium signal-to-noise spectra 4= poor quality, low signal-to-noise spectra 5= unpublished profile Width of the H_alpha line Observed width from the H_alpha rotation curves found in the literature (in km/sec), uncorrected for galaxy inclination. Central velocity dispersion from the width of the Mg I absorption triplet (lambda 5167.3, 5172.7, 5183.6) (in km/s). Measurements are from McElroy (1995) and from Scodeggio (1997), reduced homogeneously to a common aperture according to the prescriptions of Jorgensen et al. (1996). Structural parameters Concentration index C31 The ratio of the radii containing 75% and 25% of the light. This is computed in the H, V, B bands (when available). See Gavazzi et al. 2000, A&A, 361, 863 1.65 micron (H band) surface photometry of galaxies. V. Profile decompositions of 1157 galaxies. Re Effective radius containing 50% of the total asymptotic magnitude. This is computed in the H, V, B bands (when available). See Gavazzi et al. 2000, A&A, 361, 863 1.65 micron (H band) surface photometry of galaxies. V. Profile decompositions of 1157 galaxies. mu_e Effective surface brightness computed at R_e. This is computed in the H, V, B bands (when available). See Gavazzi et al. 2000, A&A, 361, 863 1.65 micron (H band) surface photometry of galaxies. V. Profile decompositions of 1157 galaxies. Total Asymptotic Magnitude Total asymptotic magnitude obtained by fitting the light curves with either exponential or de Vaucouleurs (or combination of the two) models. This is computed in the H, V, B bands (when available). See Gavazzi et al. 2000, A&A, 361, 863 1.65 micron (H band) surface photometry of galaxies. V. Profile decompositions of 1157 galaxies. Imaging Finding chart Finding Charts are available from the Digitized Palomar Sky Survey for all galaxies. Each selected galaxy appears at the center of the 10x10 arcmin^2 finding chart. When multiple catalogued galaxies appear in the same finding chart, by clicking over their names each of them can be selected. In this case the database and image queries are re-directed to the selected galaxy. B Image B band Image V Image V band Image H_alpha NET Image Halpha image obtained from the difference between the On-band narrow-band image and the Halpha OFF image (see below). H_alpha OFF Image Image of the underlying stellar continuum near H_alpha obtained either from narrow-band or broad-band (R) imaging. H Image Near Infrared H band image. K Image Near Infrared K band image. RGB Image Synthesized color RGB image obtained combining either B,V and H broad band images, or H_alpha NET, H_alpha OFF and H_alpha OFF images. Spectrum These are optical spectra integrated over the whole surface of the galaxy (obtained in drift-scan mode) as given in Gavazzi et al. 2002, ApJ, 576, 135. "Spectro-photometry of galaxies in the Virgo cluster. I: The star formation Histories". The spectra are transformed to rest-frame. The intensity is normalized to the flux at 5500 A (V band). Spectra derive from observational campaigns carried out with optical telescopes (OHP 1.9m, ESO 3.6m). See also: Gavazzi et al. (1999b, 2000d, 2002c,d,e). Light Profile Radial profiles of the light distribution as obtained on the available (B, V, H) images. See Gavazzi et al. 2000, A&A, 361, 863 1.65 micron (H band) surface photometry of galaxies. V. Profile decompositions of 1157 galaxies. When at least two radial profiles are available the color radial profile is also shown. SED These are Spectral Energy distributions from the UV to the centimetric radio continuum obtained from broad-band photometry. Notice that the data are total fluxes (extrapolated to the optical radii), unlike the individual aperture data given by NED. However the data are given as observed, i.e. uncorrected for extinction from our Galaxy and for internal extinction. The log of the Flux (in mJy) is given as a function of the log of the wavelength (in micron). SDSS Images The solid response curves show the througput defining the survey's photometric system, which includes extinction through an airmass of 1.3 at Apache Point Observatory. For reference, the dashed curves do not include any atmospheric extinction. These are sometimes loosely referred to as "filter curves" although they do include the full system response from atmosphere to detector. 
UKIDSS Images The specified transmission profiles of the WFCAM filter set, normalised to the peak transmission, plotted against wavelength. The five broad-band filters are plotted in red, and the two 1% narrow-band filters are plotted in green. The lilac line plots the atmospheric transmission (normalised to the continuum) for typical conditions.  |
