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J/AJ/121/148      Photometry of Dorado Group Dwarf Galaxies    (Carrasco+, 2001)

The dwarf galaxy population of the Dorado group down to Mv ≃ -11. Carrasco E.R., De Oliveira C.M., Infante L., Bolte M. <Astron. J., 121, 148-168 (2001)> =2001AJ....121..148C
ADC_Keywords: Photometry, CCD ; Photometry, surface ; Clusters, galaxy Keywords: Galaxies: Clusters: General, Galaxies: Clusters: Individual: Name: Dorado Group, Galaxies: Dwarf, Galaxies: Fundamental Parameters, galaxies: luminosity function Abstract: We present V and I CCD photometry of suspected low surface brightness dwarf galaxies detected in a survey covering ∼2.4 deg2 around the central region of the Dorado group of galaxies. The low surface brightness galaxies were chosen based on their sizes and magnitudes at the limiting isophote of 26Vµ. The selected galaxies have magnitudes brighter than V∼20 (MV~-11 for an assumed distance to the group of 17.2 Mpc), with central surface brightnesses µ0>22.5 Vmag.arcsec-2, scale lengths h>2", and diameters ≥14" at the limiting isophote. Using these criteria, we identified 69 dwarf galaxy candidates. Four of them are large very low surface brightness galaxies that were detected on a smoothed image, after masking high surface brightness objects. Monte Carlo simulations performed to estimate completeness, photometric uncertainties and to evaluate our ability to detect extended low surface brightness galaxies show that the completeness fraction is, on average, >80% for dwarf galaxies with -17<MV←10.5 and 22.5<µ0<25.5 Vmag.arcsec-2, for the range of sizes considered by us (D≥14"). The V-I colors of the dwarf candidates vary from -0.3 to 2.3 with a peak on V-I=0.98, suggesting a range of different stellar populations in these galaxies. The projected surface density of the dwarf galaxies shows a concentration toward the group center similar in extent to that found around five X-ray groups and the elliptical galaxy NGC 1132 studied by Mulchaey & Zabludoff (1999ApJ...514..133M), suggesting that the dwarf galaxies in Dorado are probably physically associated with the overall potential well of the group. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 84 69 Photometric Data and Profile Fit Parameters
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 9 A9 --- ID Dwarf galaxy identification 11 A1 --- f_ID [f] Indicates not detected in I filter (see section 2.7) 13 I1 h RAh Right ascension (J2000) 15- 16 I2 min RAm Right ascension (J2000) 18- 21 F4.1 s RAs Right ascension (J2000) 23 A1 --- DE- Sign of the declination (J2000) 24- 25 I2 deg DEd Declination (J2000) 27- 28 I2 arcmin DEm Declination (J2000) 30- 31 I2 arcsec DEs Declination (J2000) 33- 37 F5.2 mag Vmag Total V-band magnitude (1) 39- 43 F5.2 mag V-I ? The V-I color (1) 45- 48 F4.1 arcsec D26 Limiting isophotal diameter at 26 V mag/arcsec2 50 A1 --- f_D26 [e] Flag on D26 (2) 52- 55 F4.1 arcsec Theta26 Eq. (4) diameter at 26 V mag/arcsec2 57 A1 --- f_Theta26 [e] Flag on Theta26 (2) 59- 62 F4.1 mag/arcsec2 Mu0 Extrapolated central surface brightness in V 64- 67 F4.1 arcsec Scl Scale length 69- 72 F4.1 arcsec Rad Effective radius 74- 77 F4.1 mag/arcsec2 Mueff Mean effective surface brightness 79- 82 A4 --- Type Morphological type (see section 3.1) 84 A1 --- f_Type Flag on Type (3)
Note (1): Magnitude within 7'' and 4'' diameter apertures for CTIO and LCO40 data, respectively. Not corrected according to the simulation in section 2.6 and not corrected by interstellar absorption. Note (2): Limiting isophotal diameter and diameter given by equation (4) at the surface brightness of 26.5 V mag/arcsec2. Note (3): the flag takes the folloxing values: b = Shows knots of star formation regions; c = Red irregular galaxy; d = Extended irregular low surface brightness cloud located ∼10' to the northwest of the NGC 1549 galaxy.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Laurent Cambresy [CDS] 23-Jul-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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