J/AJ/141/23 HI holes in THINGS galaxies (Bagetakos+, 2011)
The fine-scale structure of the neutral interstellar medium in nearby galaxies.
Bagetakos I., Brinks E., Walter F., De Blok W.J.G., Usero A., Leroy A.K.,
Rich J.W., Kennicutt R.C.
<Astron. J., 141, 23 (2011)>
=2011AJ....141...23B 2011AJ....141...23B
ADC_Keywords: Galaxies, nearby ; H I data ; Morphology
Keywords: galaxies: ISM - galaxies: structure - ISM: bubbles - ISM: structure
Abstract:
We present an analysis of the properties of HI holes detected in 20
galaxies that are part of "The HI Nearby Galaxy Survey." We detected
more than 1000 holes in total in the sampled galaxies. Where they can
be measured, their sizes range from about 100pc (our resolution
limit) to about 2kpc, their expansion velocities range from 4 to
36km/s, and their ages are estimated to range between 3 and 150Myr.
The holes are found throughout the disks of the galaxies, out to the
edge of the HI disk; 23% of the holes fall outside R25. We find that
shear limits the age of holes in spirals (shear is less important in
dwarf galaxies) which explains why HI holes in dwarfs are rounder, on
average than in spirals.
Description:
The present study is based on observations carried out within the
framework of THINGS project.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 88 20 *Characteristics of the galaxies in the sample
table7.dat 85 1046 Hole properties
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Note on table2.dat: All values taken from Walter et al. (2008,
Cat. J/AJ/136/2563) unless stated otherwise.
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See also:
J/AJ/136/2563 : HI Nearby Galaxy Survey, THINGS (Walter+, 2008)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Galaxy name
13- 21 A9 --- OName Other name
23- 24 I2 h RAh Right ascension (J2000)
26- 27 I2 min RAm Right ascension (J2000)
29- 32 F4.1 s RAs Right ascension (J2000)
34 A1 --- DE- Declination sign J2000)
35- 36 I2 deg DEd Declination (J2000)
38- 39 I2 arcmin DEm Declination (J2000)
41- 44 F4.1 arcsec DEs Declination (J2000)
46- 55 A10 --- Type Morphological type
57- 60 F4.1 Mpc Dist Distance
62- 63 I2 deg Incl Average inclination
65- 67 I3 deg PA Average position angle
69- 72 F4.1 10+8Msun MHI HI mass
74- 78 F5.2 [Msun/yr] logSFR Stellar formation rate
79 A1 --- r_logSFR [cd] Reference for logSFR (1)
81- 84 F4.2 [0.1arcmin] logD25 Isophotal 25mag/arcsec2 major diameter
86- 88 I3 pc Res Resolution
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Note (1): References as follows:
c = Hunter & Elmegreen (2004, Cat. J/AJ/128/2170)
d = Hunter et al. (1999AJ....118.2184H 1999AJ....118.2184H)
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Galaxy name
13- 15 I3 --- Seq Hole index number within the galaxy,
[BBW2011] Galaxy NNN in Simbad
17- 18 I2 h RAh Hour of Right Ascension (J2000)
20- 21 I2 min RAm Minute of Right Ascension (J2000)
23- 26 F4.1 s RAs Second of Right Ascension (J2000)
28 A1 --- DE- Sign of the Declination (J2000)
29- 30 I2 deg DEd Degree of Declination (J2000)
32- 33 I2 arcmin DEm Arcminute of Declination (J2000)
35- 38 F4.1 arcsec DEs Arcsecond of Declination (J2000)
40- 43 I4 km/s HV Heliocentric velocity of center
45 I1 --- Type [1/3] Hole type; see section 4.2 (1)
47- 50 I4 pc d Diameter
52- 53 I2 km/s Vexp Expansion velocity
55- 57 I3 deg PA Position angle
59- 61 F3.1 --- Ratio Axial ratio; bmin/bmaj
63- 66 F4.1 kpc R Galactocentric radius
68- 71 F4.1 cm-3 nHI HI volume density around the hole
73- 75 I3 Myr tkin Kinetic age
77- 80 F4.1 [10+43J] log(E) Log estimated energy requirement in 1050ergs
82- 85 F4.1 [10+4Msun] logMHI Log estimated missing HI mass
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Note (1): Type as follows:
1 = it is impossible to measure an expansion velocity. However, it is very
likely that these have actually stalled and their final expansion
velocity will be equal to the velocity dispersion of the gas
2 = the expansion velocity was taken as the difference between the velocity
of the HI from that side of the hole which is seen to deviate from its
measured velocity and the mean velocity of ambient gas surrounding the
hole
3 = the expansion velocity was taken as half the difference between the
velocity of the approaching and receding sides of the hole
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 21-Jul-2012