J/MNRAS/502/5711 HI global scaling relations in WISE-WHISP (Naluminsa+, 2021)
H I global scaling relations in the WISE-WHISP survey.
Naluminsa E., Elson E.C., Jarrett T.H.
<Mon. Not. R. Astron. Soc., 502, 5711-5725 (2021)>
=2021MNRAS.502.5711N 2021MNRAS.502.5711N (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; H I data ; Star Forming Region ; Infrared
Keywords: galaxies: dwarf - galaxies: evolution - galaxies: ISM -
galaxies: spiral - galaxies: star formation
Abstract:
We present the global scaling relations between the neutral atomic
hydrogen gas, the stellar disc, and the star-forming disc in a sample
of 228 nearby galaxies that are both spatially and spectrally resolved
in HI line emission. We have used HI data from the Westerbork survey
of HI in Irregular and Spiral galaxies (WHISP) and Mid-Infrared
(3.4µm, 11.6µm) data from the Wide-field Infrared Survey
Explorer (WISE) survey, combining two data sets that are well-suited
to such a study in terms of uniformity, resolution, and sensitivity.
We utilize a novel method of deriving scaling relations for quantities
enclosed within the stellar disc rather than integrating over the HI
disc and find the global scaling relations to be tighter when defined
for enclosed quantities. We also present new HI intensity maps for the
WHISP survey derived using a robust noise rejection technique along
with corresponding velocity fields.
Description:
The sample used in this study was chosen from the WHISP 30arcsec
resolution data which have higher sensitivity to low HI column density
structures than the full resolution (14arcsecx14arcsec/sinδ)
data.
Infrared data for the sample were obtained from the WISE Extended
Source Catalogue (Jarrett et al. 2019ApJS..245...25J 2019ApJS..245...25J, Cat.
J/ApJS/245/25) which constructed native resolution mosaics and carried
out source characterization designed for large galaxies. WISE mid-IR
imaging is sensitive to stellar mass (in the short-wavelength bands)
and ISM activity (long wavelength bands). Galaxies in close
interactions (close enough for the interaction to be seen in the
infrared images) or mergers as well as poor data and non-detections
were excluded. These data were visually inspected to ensure there were
no disturbances on the target's IR flux by bright foreground stars.
Wherever the masking or subtraction of these stars adversely
compromised the disc of the galaxy that target was dropped from the
sample. These criteria resulted in a sample of 228 galaxies.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablee1.dat 54 228 Observational parameters of HI data from the
WHISP survey
tablee2.dat 62 228 HI global properties
tablee3.dat 77 228 Photometric parameters of IR data from WISE
tablee4.dat 78 180 Derived properties of the WISE data
(Jarrett et al. 2019ApJS..245...25J 2019ApJS..245...25J,
Cat. J/ApJS/245/25)
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See also:
J/ApJS/245/25 : WISE Extended Source Catalog (WXSC). I. (Jarrett+, 2019)
Byte-by-byte Description of file: tablee1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name Source name
10- 17 F8.4 deg RAdeg Right ascension (J2000)
19- 25 F7.4 deg DEdeg Declination (J2000)
27- 31 F5.2 arcsec Bmaj Beam resolution (major axis)
33- 37 F5.2 arcsec Bmin Beam resolution (minor axis)
39- 40 I2 deg BPA Beam position angle
42- 45 F4.2 mJy/beam Noise Average noise in cubes before primary beam
correction
47- 49 I3 --- Chan Number of velocity channels (1)
51- 54 F4.1 km/s DV Velocity resolution of the cube
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Note (1): Number of velocity channels, dependent on the WHISP flux density
category (<100mJy, 100mJy-300mJy, >300mJy)
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Byte-by-byte Description of file: tablee2.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name Source name
10- 15 F6.1 km/s Vsys Systemic velocity
17- 21 F5.1 km/s W20 Global profile linewidth at the 20 per cent
level
23- 27 F5.1 km/s W50 Global profile linewidth at the 50 per cent
level
29- 31 I3 arcsec RHI HI radius measured at
ΣHI=1M☉/pc2
33- 37 F5.1 Jy.km/s ISdv Integrated HI flux
39- 43 F5.2 [Msun] logMHI Logarithm of the total HI mass
45- 48 F4.2 [Msun] e_logMHI Error on logMHI
50- 53 F4.1 Mpc D Distance
55- 58 F4.1 Mpc e_D Error on D
60- 62 A3 --- r_D Reference for D (1)
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Note (1): Reference as follows:
CF2 = Cosmic flow data base (Tully et al. 2013AJ....146...86T 2013AJ....146...86T,
Cat. J/AJ/146/86)
NED = Mould flow model estimates from the NED data base
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Byte-by-byte Description of file: tablee3.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name Source name
10- 13 F4.2 --- b/a Axial ratio of the stellar disc measured in the
W1-band
15- 19 F5.1 deg PA Position angle of the stellar disc measured in
the W1-band
21- 26 F6.2 arcsec R1iso Semimajor axis of the 1σ isophote in W1
28- 32 F5.2 mag W1mag WISE W1 (3.36um) band Vega magnitude
34- 37 F4.2 mag e_W1mag Error on W1mag
39- 43 F5.2 mag W3mag ? WISE W3 (12.1um) band Vega magnitude
45- 49 F5.2 mag e_W3mag ? Error on W2mag
51- 55 F5.2 mag W4mag ? WISE W4 (22.2um) band Vega magnitude
57- 61 F5.2 mag e_W4mag ? Error on W4mag
63- 67 F5.2 mag W1-W2 ? W1-W2 colour index
69- 72 F4.2 mag W2-W3 ? W2-W3 colour index
74- 77 A4 --- Morph Morphology
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Byte-by-byte Description of file: tablee4.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name Source name
10- 13 F4.1 --- SNRW1 Signal to noise ratio on the W1-band
15- 18 F4.1 --- SNRW3 Signal to noise ratio on the W3-band
20- 23 F4.1 --- SNRW4 Signal to noise ratio on the W4-band
25- 30 F6.1 mJy FW1 Flux on the W1-band (1)
32- 37 F6.1 mJy FW3 Flux on the W3-band
39- 45 F7.1 mJy FW4 ? Flux on the W4-band
47- 51 F5.2 [Msun] logM* Logatithm of the stellar mass
53- 56 F4.2 [Msun] e_logM* Error on logM*
58- 62 F5.2 [Msun/yr] logSFRW3 Logarithm of the star formation rate from
the W3-band
64- 67 F4.2 [Msun/yr] e_logSFRW3 Error on logSFRW3
69- 73 F5.2 [Msun/yr] logSFRW4 ? Logarithm of the star formation rate
from the W4-band
75- 78 F4.2 [Msun/yr] e_logSFRW4 ? Error on logSFRW4
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Note (1): The W1 fluxes were not corrected for non-stellar sources of radiation,
hence the derived stellar masses are to be taken as upper boundaries
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 02-Nov-2023