J/ApJ/826/136 Water masers in M31. II. Multiwavelength data (Amiri+, 2016)
Water masers in the Andromeda galaxy.
II. Where do masers arise?
Amiri N., Darling J.
<Astrophys. J., 826, 136-136 (2016)>
=2016ApJ...826..136A 2016ApJ...826..136A (SIMBAD/NED BibCode)
ADC_Keywords: Masers ; Galaxies, nearby ; Infrared sources
Keywords: galaxies: individual: M31; galaxies: ISM; galaxies: star formation;
Local Group; masers; radio lines: galaxies
Abstract:
We present a comparative multiwavelength analysis of
water-maser-emitting regions and non-maser-emitting luminous 24µm
star-forming regions in the Andromeda Galaxy (M31) to identify the
sites most likely to produce luminous water masers useful for
astrometry and proper motion studies. Included in the analysis are
Spitzer 24µm photometry, Herschel 70 and 160µm photometry,
Hα emission, dust temperature, and star-formation rate. We find
significant differences between the maser-emitting and
non-maser-emitting regions: water-maser-emitting regions tend to be
more infrared-luminous and show higher star-formation rates. The five
water masers in M31 are consistent with being analogs of water masers
in Galactic star-forming regions and represent the high-luminosity
tail of a larger (and as yet undetected) population. Most regions
likely to produce water masers bright enough for proper motion
measurements using current facilities have already been surveyed, but
we suggest three ways to detect additional water masers in M31: (1)
reobserve the most luminous mid- or far-infrared sources with higher
sensitivity than was used in the Green Bank Telescope survey; (2)
observe early-stage star-forming regions selected by millimeter
continuum that have not already been selected by their 24µm
emission, and (3) reobserve the most luminous mid- or far-infrared
sources and rely on maser variability for new detections.
Description:
In this paper, we present a comparative multiwavelength analysis of
22GHz water-maser-emitting and non-maser-emitting 24um luminous
star-forming regions in M31. We use WISE, Spitzer, and Herschel
infrared continuum maps, maps of derived quantities such as star
formation and dust temperature, and archival catalogs to examine the
differences between maser-emitting and non-maser-emitting regions, to
examine correlations between observable quantities among each
population, and to constrain the parameter space most likely to
produce detectable water masers.
Throughout the manuscript, we assume a distance to M31 of 780kpc when
calculating luminosities from continuum or line flux measurements.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 135 5 Multi-wavelength properties of the water maser
hosts in M31
table3.dat 112 457 Multi-wavelength properties of the non-maser sample
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See also:
J/ApJ/826/24 : Water masers in M31. I. Recombination lines (Darling+, 2016)
J/A+A/550/A21 : Massive star-forming regions radio lines (Sanchez-Monge+, 2013)
J/ApJ/764/61 : Water maser & NH3 survey of GLIMPSE EGOs (Cyganowski+, 2013)
J/MNRAS/418/1689 : Red MSX water maser and ammonia emissions (Urquhart+, 2011)
J/AJ/142/139 : A new catalog of HII regions in M31 (Azimlu+, 2011)
J/MNRAS/416/1764 : H2O Southern Galactic Plane Survey (HOPS) (Walsh+, 2011)
J/AJ/136/2391 : GLIMPSE Extended Green Objects catalog (Cyganowski+, 2008)
J/ApJ/687/230 : Survey of M31 with Spitzer (Mould+, 2008)
J/ApJ/678/96 : Extragalactic H2O masers (Braatz+, 2008)
J/A+A/481/345 : SED evolution in massive YSOs (Molinari+, 2008)
J/MNRAS/369/120 : Kinematic survey of PNe in M31 (Merrett+, 2006)
J/AJ/131/2478 : M31 and M33 UBVRI photometry (Massey+, 2006)
J/ApJ/633/871 : Positions & photometry of HII knots in M51 (Calzetti+, 2005)
J/ApJ/581/325 : NGC 2071 water masers (Seth+, 2002)
J/MNRAS/276/57 : IRAS Galactic star-forming regions. II. (Codella+ 1995)
Byte-by-byte Description of file: table[23].dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Object identifier from J2000 position
19- 22 F4.1 K Tdust [14.3/26]? Dust temperature (1)
24- 30 F7.4 [Msun/yr] logSFR [-5.5/-3.2] Log Star Formation Rate
32- 37 F6.4 [Msun/yr] e_logSFR The 1σ uncertainty in logSFR (2)
39- 45 F7.4 [Jy] logF24 [-2.5/-0.3] Log 24 micron flux density
47- 52 F6.4 [Jy] e_logF24 The 1σ uncertainty in logF24 (2)
54 A1 --- l_logF70 Limit flag on logF70
56- 62 F7.3 [Jy] logF70 [-1.3/0.6] Log 70 micron flux density
64- 68 F5.3 [Jy] e_logF70 ? The 1σ uncertainty in logF70 (2)
70 A1 --- l_logF160 Limit flag on log160
72- 77 F6.3 [Jy] logF160 [-1.3/0.7] Log 160 micron flux density
79- 83 F5.3 [Jy] e_logF160 ? The 1σ uncertainty in logF160 (2)
85 A1 --- l_logHa Limit flag on logHa
87- 94 F8.3 [mW/m2] logHa [-16/-11.9] Log Hα line flux
96-100 F5.3 [mW/m2] e_logHa ? The 1σ uncertainty in logHa (2)
102-106 F5.3 [Lsun] logLTIR [5/6.9]? Log total IR luminosity
108-112 F5.3 [Lsun] e_logLTIR ? The 1σ uncertainty in logLTIR (2)
114-116 I3 mJy.km/s H2O [58/447]? H2O flux density
(only for table 2) (3)
118-119 I2 mJy.km/s e_H2O ? The 1σ uncertainty in H2O (2)
121-127 F7.5 Lsun LH2O [0.0008/0.007]? H2O luminosity
(only for table 2) (3)
129-135 F7.5 Lsun e_LH2O ? The 1σ uncertainty in LH2O (2)
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Note (1): The uncertainty in Tdust is 1.4K (Smith+ 2012ApJ...756...40S 2012ApJ...756...40S).
Note (2): The 1σ uncertainties for photometric flux densities and SFR
indicate statistical uncertainties for images with high signal to
noise ratios, but the systematic uncertainties are likely to be
higher.
Note (3): The integrated water maser flux densities and luminosities were
obtained from Darling (2011ApJ...732L...2D 2011ApJ...732L...2D).
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History:
From electronic version of the journal
References:
Darling J. 2011ApJ...732L...2D 2011ApJ...732L...2D
Darling et al. Paper I. 2016ApJ...826...24D 2016ApJ...826...24D Cat. J/ApJ/826/24
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 26-Sep-2016