J/A+A/581/A124 SFR IRAS 05137+3919 star and jet multiplicity (Cesaroni+, 2015)
Star and jet multiplicity in the high-mass star forming region IRAS 05137+3919.
Cesaroni R., Massi F., Arcidiacono C., Beltran M.T., Persi P., Tapia M.,
Molinari S., Testi L., Busoni L., Riccardi A., Boutsia K., Bisogni S.,
Mccarthy D., Kulesa C.
<Astron. Astrophys., 581, A124-124 (2015)>
=2015A&A...581A.124C 2015A&A...581A.124C (SIMBAD/NED BibCode)
ADC_Keywords: Associations, stellar ; Infrared sources
Keywords: stars: early-type - stars: formation - ISM: jets and outflows
Abstract:
We present a study of the complex high-mass star forming region
IRAS05137+3919 (also known as Mol8), where multiple jets and a rich
stellar cluster have been described in previous works. Our goal is to
determine the number of jets and shed light on their origin, and thus
determine the nature of the young stars powering these jets. We also
wish to analyse the stellar clusters by resolving the brightest group
of stars. The star forming region was observed in various tracers and
the results were complemented with ancillary archival data. The new
data represent a substantial improvement over previous studies both in
resolution and frequency coverage. In particular, adaptive optics
provides us with an angular resolution of 80mas in the near IR, while
new mid- and far-IR data allow us to sample the peak of the spectral
energy distribution and thus reliably estimate the bolometric
luminosity. Thanks to the near-IR continuum and millimetre line data
we can determine the structure and velocity field of the bipolar jets
and outflows in this star forming region. We also find that the stars
are grouped into three clusters and the jets originate in the richest
of these, whose luminosity is ∼2.4x104L☉. Interestingly, our
high-resolution near-IR images allow us to resolve one of the two
brightest stars (A and B) of the cluster into a double source (A1+A2).
We confirm that there are two jets and establish that they are powered
by B-type stars belonging to cluster C1. On this basis and on
morphological and kinematical arguments, we conclude that the less
extended jet is almost perpendicular to the line of sight and that it
originates in the brightest star of the cluster, while the more
extended one appears to be associated with the more extincted, double
source A1+A2. We propose that this is not a binary system, but a small
bipolar reflection nebula at the root of the large-scale jet,
outlining a still undetected circumstellar disk. The gas kinematics on
a scale of ∼0.2pc seems to support our hypothesis, because it appears
to trace rotation about the axis of the associated jet.
Description:
Near-IR images were taken in the night of December 12, 2009 with LUCI
at the Large Binocular Telescope (Mount Graham, Arizona), through the
standard broad-band filters H (λc=1.653um) and
Ks (λc=2.163um), and the narrow-band filters
FeII (λc=1.646um, including the [FeII] 1.64-um line) and
H2 (λc=2.122um, including the H2v=1-0 S(1) line at 2.12um).
Data were also collected on October 9 and 12, 2013, using the PISCES
Near Infrared Camera installed at the focal plane of the First Light
Adaptive Optics system of the Large Binocular Telescope.
Ground-based diffraction-limited mid-infrared images at 8.9, 9.9,
12.7, and 18.7um of IRAS 05137+3919 were taken on the night of
November 9, 2006 with the mid-infrared camera CID mounted on the 2.1m
telescope of the Observatorio Astronomico Nacional at San Pedro
Martir, Baja California, Mexico.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 63 1506 Coordinates, magnitudes, and colour of the
sources identified in the LUCI field
tablea2.dat 35 27 Coordinates and fluxes of the H2 knots belonging
to Jet 1
tablea3.dat 35 14 Coordinates and fluxes of the H2 knots belonging
to Jet 2
tablea4.dat 35 3 Coordinates and fluxes of the H2 knots belonging
to Jet 3
tablea5.dat 63 173 Coordinates, magnitudes, and colour of the
sources identified in the PISCES field
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea[15].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 h RAh Right ascension (J2000)
4- 5 I2 min RAm Right ascension (J2000)
7- 11 F5.2 s RAs Right ascension (J2000)
13 A1 --- DE- Declination sign (J2000)
14- 15 I2 deg DEd Declination (J2000)
17- 18 I2 arcmin DEm Declination (J2000)
20- 23 F4.1 arcsec DEs Declination (J2000)
25- 30 F6.3 mag Hmag ?=- H magnitude
32- 36 F5.3 mag e_Hmag ? rms uncertainty on Hmag
39- 44 F6.3 mag Ksmag ?=- Ks magnitude
46- 50 F5.3 mag e_Ksmag ? rms uncertainty on Ksmag
52- 57 F6.3 mag H-Ks ?=- H-Ks colour index
59- 63 F5.3 mag e_H-Ks ? rms uncertainty on H-Ks
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea[234].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 h RAh Right ascension (J2000)
4- 5 I2 min RAm Right ascension (J2000)
7- 12 F6.3 s RAs Right ascension (J2000)
14 A1 --- DE- Declination sign (J2000)
15- 16 I2 deg DEd Declination (J2000)
18- 19 I2 arcmin DEm Declination (J2000)
21- 25 F5.2 arcsec DEs Declination (J2000)
27- 31 F5.1 10-19W/m2 Flux Line emission flux on the final averaged
(mosaiced) H2 (2.122um) image
33- 35 F3.1 10-19W/m2 e_Flux rms uncertainty on Flux
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 25-Nov-2015