J/ApJS/209/25 H2O + CH3OH maser survey of Orion protostars (Kang+, 2013)
Water and methanol maser survey of protostars in the Orion molecular cloud
complex.
Kang M., Lee J.-E., Choi M., Choi Y., Kim K.-T., Di Francesco J.,
Park Y.-S.
<Astrophys. J. Suppl. Ser., 209, 25 (2013)>
=2013ApJS..209...25K 2013ApJS..209...25K
ADC_Keywords: Masers ; Infrared sources ; Radio lines ; Surveys
Keywords: ISM: jets and outflows; ISM: structure; masers; stars: formation
Abstract:
The results of a maser survey toward 99 protostars in the Orion
molecular cloud complex are presented. The target sources are low-mass
protostars identified from infrared observations. Single-dish
observations were carried out in the water maser line at 22GHz and the
methanol class I maser lines at 44, 95, and 133GHz. Most of the
detected sources were mapped to determine the source positions. Five
water maser sources were detected, and they are excited by
HH 1-2 VLA 3, HH 1-2 VLA 1, L1641N MM1/3, NGC 2071 IRS 1/3, and an
object in the OMC 3 region. The water masers showed significant
variability in intensity and velocity with time scales of 1 month or
shorter. Four methanol emission sources were detected, and those in
the OMC 2 FIR 3/4 and L1641N MM1/3 regions are probably masers. The
methanol emission from the other two sources in the NGC 2071 IRS 1-3
and V380 Ori NE regions are probably thermal. For the water masers,
the number of detections per protostar in the survey region is about
2%, which suggests that the water masers of low-mass protostars are
rarely detectable. The methanol class I maser of low-mass protostars
is an even rarer phenomenon, with a detection rate much smaller than
1%.
Description:
Out of the protostars listed in the Herschel Orion Protostar Survey
(HOPS) catalogue (Fischer et al. 2010A&A...518L.122F 2010A&A...518L.122F; Stutz et al.
2013, J/ApJ/767/36), we selected protostars showing line wings in the
CO(J=2->1) line spectra obtained with the Seoul Radio Astronomy
Observatory 6m telescope.
In the Orion molecular cloud complex 99 protostars were observed using
the KVN 21m radio antennas in the single-dish telescope mode during
the 2010 Mar-2010 Jun and 2011-2012 observing seasons. The
observations were carried out with the KVN Yonsei telescope at Seoul,
the KVN Ulsan telescope at Ulsan, and the KVN Tamna telescope at
Seogwipo, Korea.
The target lines were the H2O(616->523) (22.23508GHz) line and
the CH3OH (70->61 A+), (80->71A+), and (6-1->50E)
lines at 44.06943, 95.169516, and 132.890800GHz, respectively.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 41 6 Target sources with detections
table3.dat 41 37 Target sources affected by the Orion KL water masers
table4.dat 41 56 Target sources without a detection
table5.dat 61 34 *H2O maser line parameters
table6.dat 74 8 Line emission source positions determined by mapping
table7.dat 48 14 *CH3OH line parameters
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Note on table5.dat: The line parameters are from the Gaussian fits to each
velocity component in the spectra observed toward the target source
positions in Table 2.
Note on table7.dat: The line parameters are from the Gaussian fits to the
spectra observed toward the source positions in Table 6.
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sEe also:
J/A+A/563/A68 : CH3OH and H2O Galactic center masers (Chambers+, 2014)
J/ApJ/769/48 : Water maser in Orion-KL with Herschel (Neufeld+, 2013)
J/ApJ/767/36 : APEX observations of HOPS protostars (Stutz+, 2013)
J/AJ/144/192 : Spitzer survey of Orion A & B. I. YSO catalog (Megeath+, 2012)
J/AJ/144/31 : IR photometry of protostar candidates (Kryukova+, 2012)
J/other/RAA/10.67 : CH3OH maser sources (Liu+, 2010)
J/ApJ/710/1247 : Dense cores in Gould Belt clouds (Sadavoy+, 2010)
J/ApJ/708/758 : Polarimetry of HH1-2 region (Kwon+, 2010)
J/ApJ/702/1615 : CH3OH maser survey of EGOs (Cyganowski+, 2009)
J/A+A/496/153 : Molecular hydrogen flows along Ori A cloud (Davis+, 2009)
J/A+A/489/1409 : IR photometry and spectroscopy in L1641N (Galfalk+, 2008)
J/ApJS/155/149 : CH3OH 70-61 A+ maser sources (Kurtz+, 2004)
J/ApJ/581/325 : NGC 2071 water masers (Seth+, 2002)
J/ApJ/493/940 : Water masers in Orion (Gaume+, 1998)
J/A+A/314/615 : Maps of the 36GHz methanol emission (Liechti+, 1996)
J/AZh/72/22 : A 95GHz Survey of Methanol Masers (Valtts+, 1995)
http://www.mpia.de/homes/IRSPACE/herschel/hops/HOPS : HOPS home page
Byte-by-byte Description of file: table[234].dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- HOPS [1/362] HOPS number
5- 6 I2 h RAh Hour of right ascension (J2000)
8- 9 I2 min RAm Minute of right ascension (J2000)
11- 15 F5.2 s RAs Second of right ascension (J2000)
17 A1 --- DE- Sign of declination (J2000)
18- 19 I2 deg DEd Degree of declination (J2000)
21- 22 I2 arcmin DEm Arcminute of declination (J2000)
24- 27 F4.1 arcsec DEs Arcsecond of declination (J2000)
29- 31 A3 --- H2O [NSY, ] H2O detection? (1)
33 A1 --- CH3OH CH3OH detection? (1)
35- 37 F3.1 Jy Sig22 [0.3/0.7] Noise rms levels of the resulting
H20 spectra at 22GHz
39- 41 F3.1 Jy Sig44 [0.4/0.7] Noise rms levels of the resulting
CH3OH spectra at 44GHz
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Note (1): Code as follows:
Y = Detection
N = Non-detection
S = The H2O spectrum is affected by maser emission from the Orion KL
region coming through the beam side lobe.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1 I1 --- KLC KLC number (1)
3- 5 I3 --- HOPS [64/362] HOPS number
7- 13 A7 --- Line Line
15- 25 A11 "YYYY/MMM/DD" Epoch Epoch
26 A1 --- --- [-]
27- 28 I2 --- Day2 [1-31]? Second day of epoch
30- 35 A6 km/s Vp Peak velocity Vp
36 A1 --- n_Vp [b] b: All the velocity components
listed in Table 5
38- 39 I2 h RAh Hour of right ascension (J2000) (2)
41- 42 I2 min RAm Minute of right ascension (J2000)
44- 47 F4.1 s RAs Second of right ascension (J2000)
49 A1 --- DE- Sign of declination (J2000) (2)
50- 51 I2 deg DEd Degree of declination (J2000) (2)
53- 54 I2 arcmin DEm Arcminute of declination (J2000)
56- 57 I2 arcsec DEs Arcsecond of declination (J2000)
59- 74 A16 --- Assoc Associated object
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Note (1): The line emission sources are numbered with a prefix KLC,
<[KLC2013] N> in Simbad
Note (2): For most sources, the position uncertainty from the Gaussian
fit to the map is much smaller than the pointing uncertainty of the
telescopes, and their total position uncertainty is ∼5". For KLC 2 and 3, the
two contributions are comparable, and the total position uncertainty is ∼6".
The CH3OH source positions were determined from the maps made in the 95GHz
line.
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Byte-by-byte Description of file: table[57].dat
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Bytes Format Units Label Explanations
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1 I1 --- KLC ? KLC number (#3 in table5 was originally
marked as a footnote 'b')
3- 5 I3 --- HOPS [64/362] HOPS number
7- 9 I3 GHz Freq ? CH3OH line frequency (G1)
10 A1 --- f_Freq [b] b: two-component Gaussian fit
12- 17 F6.2 km/s Vp [-14.4/25.7] Peak velocity
19- 22 F4.2 km/s e_Vp [0.01/0.3] Vp uncertainty (2)
24- 28 F5.1 Jy.km/s FdV [0.6/311] Integrated line flux
30- 32 F3.1 Jy.km/s e_FdV [0.2/3.5] FdV uncertainty
34- 37 F4.2 km/s DelV [0.2/6.3] Line FWHM δV
39- 42 F4.2 km/s e_DelV [0.01/0.6] DelV uncertainty (2)
44- 48 F5.1 Jy Fp [1.8/395] Peak intensity from Gaussian fits
50- 60 A11 "YYYY/MMM/DD" Epoch Epoch (only for table 5)
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Note (2): When the uncertainty is smaller than 0.015km/s, it is listed
as 0.01km/s.
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Global Notes:
Note (G1): The target lines were the H2O(616->523) (22.23508GHz) line
and the CH3OH (70->61 A+), (80->71A+), and (6-1->50E)
lines at 44.06943, 95.169516, and 132.890800GHz, respectively.
History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 23-Apr-2015