J/MNRAS/483/1754 ALFALFA Low Surface Brightness Galaxy catalogue (Du+, 2019)
Low Surface Brightness Galaxy catalogue selected from the α.40-SDSS DR7
Survey and Tully-Fisher relation.
Du W., Cheng C., Wu H., Zhu M., Wang Y.
<Mon. Not. R. Astron. Soc., 483, 1754-1795 (2019)>
=2019MNRAS.483.1754D 2019MNRAS.483.1754D (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Galaxies, photometry ; Galaxies, optical ;
Magnitudes ; Morphology
Keywords: catalogues - galaxies: dwarf - galaxies: fundamental parameters -
galaxies: photometry
Abstract:
We present a catalogue of an HI-selected sample of 1129 low surface
brightness galaxies (LSBGs) searched from the α.40-SDSS DR7
survey. This sample, consisting of various types of galaxies in terms
of luminosity and morphology, has extended the parameter space covered
by the existing LSBG samples. Based on a subsample of 173 LSBGs that
are selected from our entire LSBG sample to have the 2-horn shapes of
the HI line profiles, minor-to-major axial ratios (b/a) less than 0.6
and signal-to-noise ratio of HI detection greater than 6.5, we
investigated the Tully-Fisher relation (TFr) of LSBGs in the optical
B, g, and r bands and near-infrared (NIR) J, H, and K bands as well.
In optical bands, the LSBG subsample follows the fundamental TFr that
was previously defined for normal spiral galaxies. In NIR bands, the
TFrs for our LSBG subsample are slightly different from the TFrs for
the normal bright galaxies. This might be due to the internal
extinction issue. Furthermore, the mass-to-light ratio (M/L), disc
scale length (h), and mass surface density (σ) for our LSBG
subsample were deduced from the optical TFr results. Compared with
high surface brightness galaxies (HSBGs), our LSBGs have higher M/L,
larger h, and lower σ than HSBGs.
Description:
In Du et al. (2015AJ....149..199D 2015AJ....149..199D), we have constructed a sample of
LSBGs that is searched from the α.40-SDSS DR7 survey
combination.
First of all, we reconstructed the sky background maps for SDSS DR7 g-
and r-band images for each galaxy of the entire α.40-SDSS DR7
sample (12423 galaxies). The method we used for reconstructing sky
background map is to fit the sky pixels on the object-subtracted image
row-by-row and column-by-column (Zheng et al. 1999AJ....117.2757Z 1999AJ....117.2757Z,
Cat. J/AJ/117/2757; Wu et al. 2002AJ....123.1364W 2002AJ....123.1364W), which is a better
method of constructing sky background for bright galaxies with faint
extended outskirts and in particular for LSBGs (Du et al.
2015AJ....149..199D 2015AJ....149..199D). After subtracting the sky background of
galaxies, we made surface photometry using SExtractor (Bertin &
Arnouts 1996A&AS..117..393B 1996A&AS..117..393B) and made radial profile fitting using
Galfit (Peng et al. 2002AJ....124..266P 2002AJ....124..266P). Afterwards, on the basis of
the photometric and fitting results, the g- and r-band central surface
brightness (µ0) were calculated and then converted to the B-band
values (µ0(B)). Finally, 1129 galaxies that have µ0(B)
fainter than 22.5mag/arcsec2 and minor-to-major axial ratios (b/a)
in both g and r bands larger than 0.3 were selected to be our LSBG
sample. It is an HI-selected LSBG sample, of which the data reduction,
sky subtraction, surface photometry, profile fitting, selection
criteria, and environment properties have been reported and studied in
detail in Du et al. (2015AJ....149..199D 2015AJ....149..199D). In this paper, we aim to
make the catalogue of this LSBG sample released to the public who
might be interested in this sample and also investigate the TFrs of
LSBGs in the optical and NIR bands based on this LSBG sample.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 110 1129 Catalogue of our LSBG sample from the
α.40-SDSS DR7
table2.dat 90 173 The subsample of LSBGs for optical and NIR
Tully-Fisher relation studies
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Galaxy name as it appears in the
ALFALFA (α.40) catalogue
(AGC NNNNNNA)
12- 14 I3 km/s W50 Velocity width of the HI line profile
measured at the 50 per cent level of
the peak (stemed from the α.40
catalogue)
16- 17 I2 km/s e_W50 Error on W50
19- 23 F5.2 mag gmag g-band magnitude measured on the
sky-subtracted images of galaxies
within the automatic aperture by
SExtractor (1)
25- 29 F5.3 mag e_gmag Error on gmag
31- 35 F5.2 mag rmag r-band magnitude measured on the
sky-subtracted images of galaxies
within the automatic aperture by
SExtractor (1)
37- 41 F5.3 mag e_rmag Error on rmag
43- 47 F5.2 mag Bmag B-band auto magnitude converted from
the combination of auto magnitudes in
both g and r bands (2)
49- 53 F5.3 mag e_Bmag Error on Bmag
55- 58 F4.2 --- b/a g-band major-to-minor axis ratio (b/a)
derived from fitting the
sky-subtracted image of the galaxy
with a single
exponential profile using GALFIT
60- 64 F5.2 kpc hg Disc scale length derived from fitting
the sky-subtracted image of the galaxy
with a single exponential profile
using GALFIT
66- 70 F5.2 kpc Reffg g-band effective radius given by
SExtractor
72- 76 F5.2 mag/arcsec2 SB0gAUTO g-band central surface brightness
calculated from the combination of
gmag, b/a and hg
78- 82 F5.2 mag/arcsec2 SB0BAUTO B-band central surface brightness based
on the AUTO magnitudes
84- 88 F5.2 --- SB0BISO B-band central surface brightness based
on the ISO magnitudes
90- 94 F5.2 --- SB0BISOCOR B-band central surface brightness based
on the ISOCOR magnitudes
96-100 F5.2 --- SB0BPETRO B-band central surface brightness based
on the PETRO magnitudes
102-106 F5.2 --- SB0BAVE B-band central surface brightness based
on the average of the four magnitudes
(AVE)
108 A1 --- MType Morphological type by decision trees
with random forest of machine
learning (3)
110 A1 --- LType Luminosity type in terms of B-band
absolute magnitude (4)
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Note (1): It is worth noting that SExtractor has computed several types of
magnitudes: isophotal (ISO), corrected isophotal (ISOCOR),
fixed-aperture, auto, and petrosian (PETRO) magnitudes.
Note (2): B-band auto magnitude derived using the transformation formula in
Smith et al. (2002AJ....123.2121S 2002AJ....123.2121S): Bmag=gmag+0.47(gmag-rmag)+0.17.
Note (3): Morphological classification as follows:
E = E and S0 types (2 galaxies)
S = Sa, Sab, Sb, Sbc, Sc and Scd types (151 galaxies)
L = Sd, Sm and Im types (950 galaxies)
U = Unknown type (26 galaxies)
Note (4): Luminosity type as follows:
D = Dwarf Low Surface Brightness Galaxy (LSBG) with MB>-17mag
(607 galaxies)
G = Giant Low Surface Brightness Galaxy (LSBG) with MB>-19mag
(39 galaxies)
M = Moderate-luminosity Low Surface Brightness Galaxy (LSBG) with
-19<MB←17mag (483 galaxies)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name Galaxy name as it appears in the ALFALFA
(α.40) catalogue (AGC NNNNNNA)
12- 15 F4.1 deg i Inclination angle
17- 21 F5.1 km/s W50cor Corrected velocity width of the HI line profile
measured at the 50 per cent level of the peak
23- 27 F5.2 km/s e_W50cor Error on W50cor
29- 33 F5.1 Mpc Dist Distance from the released entire ALFALFA
catalogue
35- 38 F4.2 Mpc e_Dist Error on Dist
40- 45 F6.2 mag Bmag B-band absolute magnitude that has been
corrected for Galactic and internal extinction
47- 51 F5.3 mag e_Bmag Error on Bmag
53- 58 F6.2 mag Jmag ? J-band absolute magnitude corrected only for
Galactic extinction (1)
60- 64 F5.3 mag e_Jmag ? Error on Jmag (1)
66- 71 F6.2 mag Hmag ? H-band absolute magnitude corrected only for
Galactic extinction (1)
73- 77 F5.3 mag e_Hmag ? Error on Hmag (1)
79- 84 F6.2 mag Kmag ? K-band absolute magnitude corrected only for
Galactic extinction (1)
86- 90 F5.3 mag e_Kmag ? Error on Kmag (1)
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Note (1): For those galaxies with no UKIRT Infrared Deep Sky Survey (UKIDSS)
observations, we just leave their corrected J-, H-, and K-band
absolute magnitudes blank.
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 18-Jul-2022