J/MNRAS/462/1444 MHO catalogue for Cassiopeia and Auriga (Froebrich+, 2016)
YSO jets in the Galactic plane from UWISH2.
III. Jets and outflows in Cassiopeia and Auriga.
Froebrich D., Makin S.V.
<Mon. Not. R. Astron. Soc., 462, 1444-1452 (2016)>
=2016MNRAS.462.1444F 2016MNRAS.462.1444F (SIMBAD/NED BibCode)
ADC_Keywords: YSOs ; Galactic plane ; Photometry, infrared
Keywords: stars: formation - stars: winds, outflowss -
ISM: individual: Galactic plane - ISM: jets and outflows
Abstract:
We present the analysis of 35.5deg2 of images in the 1-0 S(1) line
of H2 from the UK Widefield Infrared Survey for H2 (UWISH2)
towards Cassiopeia and Auriga. We have identified 98 Molecular
Hydrogen emission-line Objects (MHOs) driven by Young Stellar Objects,
60 per cent of which are bipolar outflows and all are new discoveries.
We estimate that the UWISH2-extended emission object catalogue
contains fewer than 2 per cent false positives and is complete at the
95 per cent level for jets and outflows brighter than the UWISH2
detection limit. We identified reliable driving source candidates for
three quarters of the detected outflows, 40 per cent of which are
associated with groups and clusters of stars. The driving source
candidates are 20 per cent protostars, the remainder are Classical
T-Tauri Stars. We also identified 15 new star cluster candidates near
MHOs in the survey area. We find that the typical outflow identified
in the sample has the following characteristics: the position angles
are randomly orientated; bipolar outflows are straight within a few
degrees; the two lobes are slightly asymmetrical in length and
brightness; the length and brightness of the lobes are not correlated;
typical time gaps between major ejections of material are 1-3 kyr,
hence FU-Ori or EX-Ori eruptions are most likely not the cause of
these, but we suggest MNors as a possible source. Furthermore, we find
that outflow lobe length distributions are statistically different
from the widely used total length distributions. There are a larger
than expected number of bright outflows indicating that the flux
distribution does not follow a power law.
Description:
Our analysis uses data from the UKIRT Widefield Infrared Survey for
H2 by Froebrich et al. (2011MNRAS.413..480F 2011MNRAS.413..480F) and its extension
towards the Cygnus X and Cassiopeia/Auriga regions discussed in
Froebrich et al. (2015, Cat. J/MNRAS/454/2586). All images are taken
with the Wide Field Camera at the UK InfraRed Telescope. A total
exposure time of 720s per pixel was obtained through the 1-0 S(1)
filter at 2.122um. Utilizing micro-stepping during the observations,
the final images have a pixel size of 0.2arcsec x 0.2arcsec and the
typical seeing in the data is 0.8 arcsec. Averaged over this typical
seeing, the typical 5σ surface brightness detection limit in the
data is 4.1x10-19W/m2/arcsec2.
In this paper, we only analyse the data taken towards the region of
Cassiopeia and Auriga.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 163 98 Summary table of the MHO properties and their
respective candidate driving sources
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See also:
J/MNRAS/454/2586 : UWISH2 extended H2 emission line sources (Froebrich+, 2015)
J/MNRAS/421/3257 : MHO catalogue for Serpens and Aquila (Ioannidis+, 2012)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 3 A3 --- --- [MHO]
4- 7 I4 --- MHO MHO number
9- 16 F8.5 deg RAdeg Right ascension (J2000)
18- 26 F9.6 deg DEdeg Declination (J2000)
28- 34 F7.5 deg Length1 ?=- Lenght of the first outflow lobe
36- 42 F7.5 deg Length2 ?=- Lenght of the second outflow lobe
44- 48 F5.1 deg PA1 ?=- Position angle of the first outflow lobe
from North over East
50- 54 F5.1 deg PA2 ?=- Position angle of the second outflow lobe
from North over East
56- 59 I4 10-19W/m2 Flux1 Integrated flux of the 1-0 S(1) line of H2
of the first outflow lobe or knot
61- 63 I3 10-19W/m2 Flux2 ?=- Integrated flux of the 1-0 S(1) line of
H2 of the second outflow lobe or knot
65 A1 --- Type [BSK] Type of outflow (1)
67 A1 --- Cl [Y/N] Is the MHO associated with cluster or
group of stars?
69- 87 A19 --- Source Source candidate identification
(or noname or unknown)
89- 90 I2 % PS ?=- Likelihood PS that source candidate
is the real driving source
92- 96 F5.2 mag Jmag1 ?=- UKIDSS J magnitude of the source
candidate (2)
98-102 F5.2 mag Jmag2 ?=- 2MASS J magnitude of the source
candidate (2)
104-108 F5.2 mag Hmag1 ?=- UKIDSS H magnitude of the source
candidate (2)
110-114 F5.2 mag Hmag2 ?=- 2MASS H magnitude of the source
candidate (2)
116-120 F5.2 mag Kmag1 ?=- UKIDSS K magnitude of the source
candidate (2)
122-126 F5.2 mag Kmag2 ?=- 2MASS K magnitude of the source
candidate (2)
128-133 F6.3 mag W1mag ?=- Wise W1 magnitude of the source candidate
135-140 F6.3 mag W2mag ?=- Wise W2 magnitude of the source candidate
142-147 F6.3 mag W3mag ?=- Wise W3 magnitude of the source candidate
149-153 F5.3 mag W4mag ?=- Wise W4 magnitude of the source candidate
155 A1 --- G [Y/N] Is the detection of the source candidate
in UKIDSS ?
157 A1 --- T [Y/N] Is the detection of the source candidate
in 2MASS ?
159 A1 --- W [Y/N] Is the detection of the source candidate
in WISE ?
161 A1 --- A [Y/N] Is the detection of the source candidate
in AKARI ?
163 A1 --- I [Y/N] Is the detection of the source candidate
in IRAS ?
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Note (1): Type of outflow as follows:
B = bipolar
S = single-sided
K = single or group of knots without apparent source candidate
Note (2): Note that same 2MASS detections might be blends of several sources.
There are 4 objects with 2GPS K-band epochs, we only list the first one in
these cases as there is no variability above the 0.1mag level between the
two epochs in all cases.
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History:
From electronic version of the journal
References:
Ioannidis & Froebrich, Paper I 2012MNRAS.421.3257I 2012MNRAS.421.3257I, Cat J/MNRAS/421/3257
Ioannidis & Froebrich, Paper II 2012MNRAS.425.1380I 2012MNRAS.425.1380I
Makin & Froebrich, Paper IV 2018ApJS..234....8M 2018ApJS..234....8M
(End) Patricia Vannier [CDS] 30-Jan-2018