J/ApJ/856/52 Kinematic distances of star-forming regions (Wenger+, 2018)
Kinematic distances: a Monte Carlo Method.
Wenger T.V., Balser D.S., Anderson L.D., Bania T.M.
<Astrophys. J., 856, 52-52 (2018)>
=2018ApJ...856...52W 2018ApJ...856...52W (SIMBAD/NED BibCode)
ADC_Keywords: H II regions; Stars, giant; Stars, distances; Radio sources;
Parallaxes, trigonometric; Milky Way; Star Forming Region
Keywords: Galaxy: kinematics and dynamics; Galaxy: structure; H II regions
ISM: kinematics and dynamics; parallaxes; radio lines: ISM
Abstract:
Distances to high-mass star-forming regions (HMSFRs) in the Milky Way
are a crucial constraint on the structure of the Galaxy. Only
kinematic distances are available for a majority of the HMSFRs in the
Milky Way. Here, we compare the kinematic and parallax distances of
75 Galactic HMSFRs to assess the accuracy of kinematic distances. We
derive the kinematic distances using three different methods: the
traditional method using the Brand & Blitz (1993, J/A+A/275/67)
rotation curve (Method A), the traditional method using the
Reid+ (2014, J/ApJ/783/130) rotation curve and updated solar motion
parameters (Method B), and a Monte Carlo technique (Method C). Methods
B and C produce kinematic distances closest to the parallax distances,
with median differences of 13% (0.43kpc) and 17% (0.42kpc),
respectively. Except in the vicinity of the tangent point, the
kinematic distance uncertainties derived by Method C are smaller than
those of Methods A and B. In a large region of the Galaxy, the Method
C kinematic distances constrain both the distances and the
Galactocentric positions of HMSFRs more accurately than parallax
distances. Beyond the tangent point along l=30°, for example, the
Method C kinematic distance uncertainties reach a minimum of 10% of
the parallax distance uncertainty at a distance of 14kpc. We develop a
prescription for deriving and applying the Method C kinematic
distances and distance uncertainties. The code to generate the Method
C kinematic distances is publicly available and may be utilized
through an online tool.
Description:
Our sample of high-mass star-forming regions (HMSFRs) comes from the
maser parallax catalog in Reid+ (2014, J/ApJ/783/130) that contains
parallaxes and proper motions for 103 HMSFRs and HMSFR proxies in the
Milky Way. These data stem from measurements made using the NRAO VLBA,
the Japanese VLBI Exploration of Radio Astrometry (VERA) project, and
the European VLBI Network (EVN).
Our final sample contains 72 HMSFRs and 3 red supergiants (HMSFR proxies).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 85 75 High-mass star-forming region (HMSFR) sample
table3.dat 73 75 Monte Carlo parallax and derived kinematic distances
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See also:
VIII/54 : Atlas of Galactic Neutral Hydrogen (Hartmann+, 1997)
VIII/75 : HI survey of the sky DE<+25° (Bajaja+, 2005)
VIII/76 : Leiden/Argentine/Bonn (LAB) Survey of Galactic HI (Kalberla+ 2005)
J/A+A/275/67 : Velocity Field of the outer Galaxy (Brand+ 1993)
J/ApJS/138/63 : H2CO and Hα observations of UC HII (Araya+, 2002)
J/ApJ/582/756 : Velocities of HII regions (Kolpak+, 2003)
J/ApJ/587/714 : H2CO and Hα observations of UC HII (Watson+, 2003)
J/ApJS/154/553 : Inner galaxy massive star formation regions (Sewilo+, 2004)
J/ApJ/690/706 : Distances of Galactic HII regions (Anderson+, 2009)
J/ApJ/699/1153 : Kinematic dist. to GRS molecular clouds (Roman-Duval+, 2009)
J/ApJ/720/1055 : VBLA observations of W51 Main/South (Sato+, 2010)
J/MNRAS/411/705 : Spectrophotometric distances of HII regions (Moises+, 2011)
J/MNRAS/420/1656 : RMS compact HII regions distances (Urquhart+, 2012)
J/ApJ/754/62 : HRDS III. HII region kinematic distances (Anderson+, 2012)
J/ApJ/783/130 : Parallaxes of high mass star forming regions (Reid+, 2014)
J/ApJS/211/29 : Atlas of HI abs. toward HII regions in SGPS I (Brown+, 2014)
J/ApJS/212/1 : The WISE catalog of Galactic HII regions (Anderson+, 2014)
J/ApJ/806/199 : RRL & continuum data of 21 Gal. HII regions (Balser+, 2015)
J/ApJS/221/26 : Radio obs. of Galactic WISE HII regions (Anderson+, 2015)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 A13 --- Name Name (GLLL.ll+BB.bb) (1)
15 A1 --- f_Name [a] a: red supergiants
17- 31 A15 --- AName Alternative name (1)
33- 34 I2 h RAh Hour of right ascension (J2000) (1)
36- 37 I2 min RAm Minute of right ascension (J2000)
39- 43 F5.2 s RAs Second of right ascension (J2000)
45 A1 --- DE- Sign of declination (J2000) (1)
46- 47 I2 deg DEd Degree of declination (J2000) (1)
49- 50 I2 arcmin DEm Arcminute of declination (J2000)
52- 55 F4.1 arcsec DEs Arcsecond of declination (J2000)
57- 61 F5.3 mas plx [0.09/2.41] Parallax (1)
63- 67 F5.3 mas e_plx [0.005/0.153] Parallax uncertainty (1)
69- 71 I3 km/s Vlsr [-73/109] Local Standard of Rest velocity (1)
73- 74 I2 km/s e_Vlsr [3/10] Vlsr uncertainty (1)
76- 85 A10 --- Ref Reference(s) (1)(2)
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Note (1): The positions, parallaxes, and LSR velocities (VLSR) from the
Reid+ (2014, J/ApJ/783/130) catalog (<[RMB2014] GLLL.ll+BB.bb> in Simbad).
Note (2): References as follows:
1 = BeSSeL Survey unpublished;
2 = Wu et al. (2014A&A...566A..17W 2014A&A...566A..17W)
4 = Sato et al. (2014ApJ...793...72S 2014ApJ...793...72S)
6 = Zhang et al. (2014ApJ...781...89Z 2014ApJ...781...89Z)
7 = Sanna et al. (2014ApJ...781..108S 2014ApJ...781..108S)
10 = Xu et al. (2011ApJ...733...25X 2011ApJ...733...25X)
11 = Brunthaler et al. (2009ApJ...693..424B 2009ApJ...693..424B)
12 = Bartkiewicz et al. (2008A&A...490..787B 2008A&A...490..787B)
13 = Kurayama et al. (2011PASJ...63..513K 2011PASJ...63..513K)
14 = Zhang et al. (2009ApJ...693..419Z 2009ApJ...693..419Z)
15 = Zhang et al. (2013ApJ...775...79Z 2013ApJ...775...79Z)
16 = Xu et al. (2009ApJ...693..413X 2009ApJ...693..413X)
17 = Sato et al. (2010ApJ...720.1055S 2010ApJ...720.1055S)
18 = Oh et al. (2010PASJ...62..101O 2010PASJ...62..101O)
19 = Rygl et al. (2010A&A...511A...2R 2010A&A...511A...2R)
20 = Nagayama et al. (2011PASJ...63...23N 2011PASJ...63...23N)
21 = Xu et al. (2013ApJ...769...15X 2013ApJ...769...15X)
22 = Sanna et al. (2012ApJ...745...82S 2012ApJ...745...82S)
23 = Ando et al. (2011PASJ...63...45A 2011PASJ...63...45A)
24 = Moscadelli et al. (2011A&A...526A..66M 2011A&A...526A..66M)
25 = Rygl et al. (2012A&A...539A..79R 2012A&A...539A..79R)
26 = Zhang et al. (2012A&A...544A..42Z 2012A&A...544A..42Z)
27 = Hachisuka et al. (2015ApJ...800....2H 2015ApJ...800....2H)
28 = Choi et al. (2014ApJ...790...99C 2014ApJ...790...99C)
29 = Hirota et al. (2008PASJ...60..961H 2008PASJ...60..961H)
30 = Moscadelli et al. (2009ApJ...693..406M 2009ApJ...693..406M)
31 = Moellenbrock et al. (2009ApJ...694..192M 2009ApJ...694..192M)
32 = Sato et al. (2008PASJ...60..975S 2008PASJ...60..975S)
33 = Xu et al. (2006Sci...311...54X 2006Sci...311...54X)
34 = Hachisuka et al. (2006ApJ...645..337H 2006ApJ...645..337H)
35 = Asaki et al. (2010ApJ...721..267A 2010ApJ...721..267A)
36 = Hachisuka et al. (2009ApJ...696.1981H 2009ApJ...696.1981H)
40 = Reid et al. (2009ApJ...693..397R 2009ApJ...693..397R)
43 = Sandstrom et al. (2007ApJ...667.1161S 2007ApJ...667.1161S)
44 = Menten et al. (2007A&A...474..515M 2007A&A...474..515M)
45 = Kim et al. (2008PASJ...60..991K 2008PASJ...60..991K)
46 = Choi et al. (2008PASJ...60.1007C 2008PASJ...60.1007C)
47 = Zhang et al. (2012ApJ...744...23Z 2012ApJ...744...23Z)
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Name HMSFR name (GLLL.ll+BB.bb)
15- 19 F5.2 kpc plxDP [0.4/11] The Monte Carlo parallax distance, DP
21- 24 F4.2 kpc e_plxDP [0.01/1.91] Lower uncertainty on plxDP
26- 29 F4.2 kpc E_plxDP [0.01/3.34] Upper uncertainty on plxDP
31- 35 F5.2 kpc DistA [0.44/11.8] The kinematic distance
using method A, DA
37- 40 F4.2 kpc e_DistA [0.3/6] DistA uncertainty
42 A1 --- KDARA Associated kinematic distance ambiguity
resolution, KDARA
44- 48 F5.2 kpc DistB [0.24/11.6] The kinematic distance
using method B, DB
50- 53 F4.2 kpc e_DistB [0.36/5.87] DistB uncertainty
55 A1 --- KDARB Associated kinematic distance ambiguity
resolution, KDARA
57- 61 F5.2 kpc DistC [0.07/11.4] The kinematic distance
using method C, DC
63- 66 F4.2 kpc e_DistC [0.06/2.4] Lower uncertainty on DistC
68- 71 F4.2 kpc E_DistC [0.31/3.3] Upper uncertainty on DistC
73 A1 --- KDARC Associated kinematic distance ambiguity
resolution, KDARC
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 03-Oct-2023