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J/ApJ/716/942       Bulges of nearby galaxies with Spitzer       (Fisher+, 2010)

Bulges of nearby galaxies with Spitzer: scaling relations in pseudobulges and classical bulges. Fisher D.B., Drory N. <Astrophys. J., 716, 942-969 (2010)> =2010ApJ...716..942F
ADC_Keywords: Galaxies, nearby ; Photometry, infrared ; Morphology Keywords: galaxies: bulges - galaxies: evolution - galaxies: formation - galaxies: fundamental parameters - galaxies: structure Abstract: We investigate scaling relations of bulges using bulge-disk decompositions at 3.6um and present bulge classifications for 173 E-Sd galaxies within 20Mpc. Pseudobulges and classical bulges are identified using Sersic index, Hubble Space Telescope morphology, and star formation activity (traced by 8um emission). In the near-IR pseudobulges have nb<2 and classical bulges have nb>2, as found in the optical. Sersic index and morphology are essentially equivalent properties for bulge classification purposes. We confirm, using a much more robust sample, that the Sersic index of pseudobulges is uncorrelated with other bulge structural properties, unlike for classical bulges and elliptical galaxies. Also, the half-light radius of pseudobulges is not correlated with any other bulge property. We also find a new correlation between surface brightness and pseudobulge luminosity; pseudobulges become more luminous as they become more dense. Description: We use data from Spitzer to perform bulge-disk decompositions at 3.6um, where the data are less affected by gradients in dust and stellar populations than in the optical bands. Also, we use 8um mid-IR data to estimate star formation rates. We also wish to compare the location of pseudobulges and classical bulges in parameter space to that of elliptical galaxies. We therefore include a set of elliptical galaxies as a control sample from Kormendy et al. (2009, Cat. J/ApJS/182/216). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 41 145 Sample galaxy properties table2.dat 92 145 Derived parameters
See also: VII/155 : Third Reference Cat. of Bright Galaxies (RC3) (de Vaucouleurs+ 1991) VII/145 : Nearby Galaxies Catalogue (NBG) (Tully 1988) J/ApJS/182/216 : Surface photometry of Virgo ellipticals (Kormendy+, 2009) J/AJ/136/773 : Structure of classical bulges and pseudobulges (Fisher+, 2008) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Name Galaxy name 10- 16 A7 --- Type Morphological type taken from RC3 18- 22 F5.2 Mpc Dist Distance 24 I1 --- r_Dist Distance reference (1) 26- 31 F6.2 mag BMag Absolute B-band magnitude 33- 36 F4.2 mag B-V ? B-V color index 38- 41 F4.2 [pc] logD25 Isophotal diameter
Note (1): Distance reference as follows: 1 = Tully & Fisher 1988cng..book.....T (see also VII/145); 2 = Tonry et al. 2001ApJ...546..681T; 3 = de Vaucouleurs et al. 1991, Cat. VII/155 (RC3)
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Name Galaxy name 10 A1 --- B [P/C/ ] Bulge morphology: P=pseudobulge, C=classical bulge 12- 15 F4.2 --- nb The bulge Sersic index 17- 20 F4.2 --- e_nb nb uncertainty 22- 27 F6.2 mag M3.6 3.6um magnitude of the bulge (M3.6Sersic) 29- 32 F4.2 mag e_M3.6 M3.6 uncertainty 34- 37 F4.2 [pc] log(re) Log of the half-light radius re 39- 42 F4.2 [pc] e_log(re) log(re) uncertainty 44- 48 F5.2 mag/arcsec2 mue The average surface brightness within the half-light radius (2) 50- 53 F4.2 mag/arcsec2 e_mue mue uncertainty 55- 59 F5.2 mag/arcsec2 mud Surface brightness (µdisk0,3.6) 61- 64 F4.2 mag/arcsec2 e_mud mud uncertainty 66- 69 F4.2 [pc] log(h) Log of the scale length of the outer disk 71- 74 F4.2 [pc] e_log(h) log(h) uncertainty 76- 81 F6.2 mag M8 ? 8um magnitude of the bulge, dominated by dust emission (M8,dust) (3) 83- 87 F5.2 mag 3.6-8 ? M3.6-M8.0_ mid-IR color index 89- 92 F4.2 mag e_3.6-8 ? 3.6-8 uncertainty
Note (2): The average surface brightness within the half-light radius, <µe> is given by <µe≥m3.6+2.5log(πre2) where m3.6 is the magnitude in 3.6um. See section 3.2 for further details. Note (3): We calculate M8,dust using the relation from Helou et al. (2004ApJS..154..253H), where M8,dust=-2.5xlog10(L8-0.232xL3.6) where L3.6 is the bulge luminosity at 3.6um. See section 6.1 for further details.
History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 31-May-2012
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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