J/MNRAS/479/3509 LVHIS. far-infrared radio correlation (Shao+, 2018)
Local Volume HI Survey: the far-infrared radio correlation.
Shao L., Koribalski B.S., Wang J., Ho L.C., Staveley-Smith L.
<Mon. Not. R. Astron. Soc. 479, 3509 (2018)>
=2018MNRAS.479.3509S 2018MNRAS.479.3509S (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Galaxies, IR ; Galaxies, radio ; H I data ; Morphology ;
Ultraviolet
Keywords: galaxies: dwarf - galaxies: photometry - galaxies: star formation -
radio continuum: galaxies - infrared: galaxies
Abstract:
In this paper we measure the far-infrared (FIR) and radio flux
densities of a sample of 82 local gas-rich galaxies, including 70
"dwarf" galaxies (M*<109M☉), from the Local Volume HI Survey
(LVHIS), which is close to volume limited. It is found that LVHIS
galaxies hold a tight linear FIR-radio correlation (FRC) over four
orders of magnitude. However, for detected galaxies only, a trend of
larger FIR-to-radio ratio with decreasing flux density is observed. We
estimate the star formation rate by combining UV and mid-IR data using
empirical calibration. It is confirmed that both FIR and radio
emission are strongly connected with star formation but with
significant non-linearity. Dwarf galaxies are found radiation
deficient in both bands, when normalized by star formation rate. It
urges a "conspiracy" to keep the FIR-to-radio ratio generally
constant. By using partial correlation coefficient in Pearson
definition, we identify the key galaxy properties associated with the
FIR and radio deficiency. Some major factors, such as stellar mass
surface density, will cancel out when taking the ratio between FIR and
radio fluxes. The remaining factors, such as HI-to-stellar mass ratio
and galaxy size, are expected to cancel each other due to the
distribution of galaxies in the parameter space. Such cancellation is
probably responsible for the "conspiracy" to keep the FRC alive.
Description:
LVHIS is a southern sky survey for all HI -rich nearby galaxies
carried out with the Australia Telescope Compact Array (ATCA). ATCA is
a radio telescope array of six 22m diameter dishes, located near
Narrabri in New South Wales, Australia. The primary beam size is
33.6-arcmin at 1.4GHz. The longest baseline is 6km , giving highest
spatial resolution around 7-arcsec at 1.4GHz.
FIR: IRAS data processed with SCANPI v6.0.
Radio: ATCA data processed with Miriad v1.5.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 76 82 Basic properties of the LVHIS sample
table2.dat 103 82 Flux measurements of LVHIS galaxies
table4.dat 102 17 Derived galaxy properties of gold sample
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See also:
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- --- [LVHIS]
7- 9 I03 --- LVHIS [001/082] LVHIS ID
11- 25 A15 --- Name Optical counterpart
27- 34 A8 --- HIPASS HIPASS ID
36- 43 F8.4 deg RAdeg Right ascension (J2000)
45- 53 F9.5 deg DEdeg Declination (J2000)
55- 58 F4.2 Mpc Dist Distance
60- 65 A6 --- MType Morphological type
67- 71 F5.2 [Msun] logMstar ? Stellar mass
73- 76 F4.2 [Msun] logMHI ? HI mass
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- --- [LVHIS]
7- 9 I03 --- LVHIS [001/082] LVHIS ID
11- 15 F5.3 mJy/beam rms ? 1.4GHz image rms
17- 21 F5.1 arcsec AperMaj ? Major axis of photometry aperture
23- 27 F5.1 arcsec AperMin ? Minor axis of photometry aperture
29- 31 I3 deg AperPA ? Position angle of photometry aperture
33 A1 --- l_F1.4 Upper limit flag of 1.4GHz flux density
35- 41 F7.2 mJy F1.4 ? 1.4GHz flux density
43- 48 F6.2 mJy e_F1.4 ? Uncertainty of 1.4GHz flux density
50 A1 --- f_F1.4 [0-5] Measurement flag of 1.4GHz flux
density (1)
52 A1 --- r_F1.4 [a-f] Literature reference of 1.4GHz flux
density (2)
54 A1 --- l_F60 Upper limit flag of 60um flux density
56- 63 F8.3 Jy F60 ? 60 micron flux density
65- 70 F6.2 Jy e_F60 ? Uncertainty of 60um flux density
72 A1 --- l_F100 Upper limit flag of 100um flux density
74- 80 F7.2 Jy F100 ? 100 micron flux density
82- 87 F6.2 Jy e_F100 ? Uncertainty of 100um flux density
89 A1 --- l_FFIR Upper limit flag of FIR flux density
91- 97 F7.2 10-14W/m2 FFIR ? FIR flux density
99-103 F5.1 10-14W/m2 e_FFIR ? Uncertainty of FIR flux density
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Note (1): Flag of Flux at a.4GHz as follows:
0 = no broad band data
1 = aperture flux density
2 = sfind flux density
3 = aperture upper limit
4 = 3-sigma upper limit (assuming point source)
5 = literature
Note (2): References as follows:
a = Condon et al., 1996ApJS..103...81C 1996ApJS..103...81C
b = Williams & Bower, 2010ApJ...710.1462W 2010ApJ...710.1462W
c = Cannon & Skillman, 2004ApJ...610..772C 2004ApJ...610..772C
d = Elmouttie et al., 1997MNRAS.284..830E 1997MNRAS.284..830E
e = Tingay et al., 2003, Cat. J/PASJ/55/351
f = Wright & Otrupcek, 1990, Cat. VIII/15
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- --- [LVHIS]
7- 9 I03 --- LVHIS [001/082] LVHIS ID
11- 22 A12 --- Name Optical counterpart
24- 28 F5.2 [Msun] logMstar Stellar mass
30- 33 F4.2 [Msun] e_logMstar Uncertainty of stellar mass
35- 39 F5.2 [Msun/yr] logSFR Star formation rate
41- 44 F4.2 [Msun/yr] e_logSFR Uncertainty of tar formation rate
46- 49 F4.2 [Msun] logMHI HI mass
51- 54 F4.2 [Msun] e_logMHI Uncertainty of HI mass
56- 58 F3.1 --- cons Stellar light concentration
60- 62 F3.1 --- e_cons Uncertainty of stellar light
concentration
64- 67 F4.1 kpc D25 25mag/arcsec^2 diameter in B band
69- 71 F3.1 kpc e_D25 Uncertainty of 25mag/arcsec^2 diameter
in B band
73- 76 F4.2 kpc RUV FUV 50 percent light radius
78- 81 F4.2 kpc e_RUV Uncertainty of FUV 50 percent light
radius
83- 86 F4.2 [Msun/kpc2] logmustar Stellar mass surface density
88- 91 F4.2 [Msun/kpc2] e_logmustar Uncertainty of stellar mass surface
density
93- 97 F5.2 [Msun/yr/kpc2] logmuSFR Star formation rate surface density
99-102 F4.2 [Msun/yr/kpc2] e_logmuSFR Uncertainty of star formation rate
surface density
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Acknowledgements:
Li Shao, lishao(at)pku.edu.cn
(End) Li Shao [CSIRO/ANU], Patricia Vannier [CDS] 17-Sep-2018