J/A+A/682/A2 AFGL 5180 ALMA, LUCI and HST images (Crowe+, 2024)
Near-infrared observations of outflows and young stellar objects in the massive
star-forming region AFGL 5180.
Crowe S., Fedriani R., Tan J.C., Whittle M., Zhang Y., Caratti o Garatti A.,
Farias J.P., Gautam A., Telkamp Z., Rothberg B., Grudic M., Andersen M.,
Cosentino G., Garcia-Lopez R., Rosero V., Tanaka K., Pinna E., Rossi F.,
Miller D., Agapito G., Plantet C., Ghose E., Christou J., Power J.,
Puglisi A., Briguglio R., Brusa G., Taylor G., Zhang X., Mazzoni T.,
Bonaglia M., Esposito S., Veillet C.
<Astron. Astrophys. 682, A2 (2024)>
=2024A&A...682A...2C 2024A&A...682A...2C (SIMBAD/NED BibCode)
ADC_Keywords: Star Forming Region ; Infrared ; Millimetric/submm sources
Keywords: techniques: high angular resolution - stars: formation -
stars: individual: AFGL 5180 - stars: protostars -
ISM: jets and outflows - infrared: stars
Abstract:
Massive stars play important roles throughout the universe; however,
their formation remains poorly understood. Observations of jets and
outflows in high-mass star-forming regions, as well as surveys of
young stellar object (YSO) content, can help test theoretical models
of massive star formation.
We aim at characterizing the massive star-forming region AFGL 5180 in
the near-infrared (NIR), identifying outflows and relating these to
sub-mm/mm sources, as well as surveying the overall YSO surface number
density to compare to massives tar formation models.
Broad- and narrow-band imaging of AFGL 5180 was made in the NIR with
the Large Binocular Telescope, in both seeing-limited (∼0.5") and high
angular resolution (∼0.09") Adaptive Optics (AO) modes, as well as
with the Hubble Space Telescope. Archival continuum data from the
Atacama Millimeter/Submillimeter Array (ALMA) was also utilized.
At least 40 jet knots were identified via NIR emission from H2 and
[FeII] tracing shocked gas. Bright jet knots outflowing from the
central most massive protostar, S4 (estimated mass ∼11M☉, via
SED fitting), are detected towards the east of the source and are
resolved in fine detail with the AO imaging. Additional knots are
distributed throughout the field, likely indicating the presence of
multiple driving sources. Sub-millimeter sources detected by ALMA are
shown to be grouped in two main complexes, AFGL 5180 M and a small
cluster ∼15" (0.15pc in projection) to the south, AFGL 5180 S. From
our NIR continuum images we identify YSO candidates down to masses of
∼0.1M☉. Combined with the sub-mm sources, this yields a surface
number density of such YSOs of N*∼103pc-2^ within a projected
radius of about 0.1pc. Such a value is similar to those predicted by
models of both Core Accretion from a turbulent clump environment and
Competitive Accretion. The radial profile of N* is relatively flat
on scales out to 0.2pc, with only modest enhancement around the
massive protostar inside 0.05pc, which provides additional
constraints on these massive star formation models.
This study demonstrates the utility of high-resolution NIR imaging, in
particular with AO, for detecting outflow activity and YSOs in distant
regions. The presented images reveal the complex morphology of
outflow-shocked gas within the large-scale bipolar flow of a massive
protostar, as well as clear evidence for several other outflow driving
sources in the region. Finally, this work presents a novel approach to
compare the observed YSO surface number density from our study against
different models of massive star formation.
Description:
Three sets of data are given below, from the Large Binocular Telescope
(LBT), Hubble Space Telescope (HST), and Atacama Large
Millimeter/Submillimeter Array (ALMA). The data are described in
sections below, with text extracted from the paper.
(1) Reduced images from the Large Binocular Telescope (LBT) of the
AFGL 5180 massive star-forming region. Observations were taken on the
10th of October, 2020 with the Large Binocular Telescope (LBT) in
binocular mode, i.e. utilizing both mirrors simultaneously, with the
LBT Utility Camera in the Infrared (LUCI; Seifert et al., 2003, in
Society of Photo- Optical Instrumentation Engineers (SPIE) Conference
Series, Vol. 4841, Instrument Design and Performance for
Optical/Infrared Ground-based Telescopes, ed. M. Iye & A. F. M.
Moorwood, 962-973) instrument in seeing limited mode (UV-2020B-04; PI:
J. C. Tan). The N3.75 camera with a pixel scale of 0.12" and (FOV) of
4'x4' was used. The filters K and Br-gamma, which are centered at the
wavelengths 2.194 and 2.170 microns, respectively, were employed on
the LUCI1 instrument mounted on the left (SX) mirror, and the filters
K and H2, which are centered at the wavelengths 2.194 and 2.124
microns, respectively, were employed on the LUCI2 instrument mounted
on the right (DX) mirror. The central coordinates of the image are
RA(J2000)=06:08:53.60, Dec(J2000)=+21:38:15.61. The images have a
position angle (PA) of 0 degrees.
Observations were also taken on the 3rd of November, 2020 with the
LUCI-1 instrument (see previous paragraph) in the Adaptive Optics (AO)
assisted mode with the Single conjugated adaptive Optics Upgrade for
the LBT (SOUL; Pinna et al. 2016, in Society of Photo-Optical
Instrumentation Engineers (SPIE) Conference Series, Vol. 9909,
Adaptive Optics Systems V, ed. E. Marchetti, L. M. Close, & J.-P.
Veran, 99093V) as part of the SOUL Commissioning Science Run scheduled
for November 1-6, 2020 (UV-2020B-501; PI: J. C. Tan). The N30 camera
with a pixel scale of 0.015" and FOV of 30"x30" was used. The filters
K, H2, and Br-gamma which are centred at the wavelengths 2.194, 2.124,
2.170 microns, respectively, were employed on the LUCI-1 instrument
mounted on the left (SX) mirror. The central coordinates of the image
were RA(J2000)=06:08:54.042, Dec(J2000)=+21:38:26.920. The AO guide
star used, 082-000146 (RA(J2000)=06:08:54.271,
Dec(J2000)=+21:38:24.324, R=15.41mag), was located at 4.2" from the
center of the image. The images were taken with a PA of 150 degrees,
though the final images used for analysis were rotated to a
PA=0 degrees. The data were reduced with custom python scripts using
the python packages ccdproc (Craig et al. 2022, ccdproc: 2.3.1 -
fixes astropy 5.1 compatibility, Zenodo), astropy (Astropy
Collaboration et al. 2022ApJ...935..167A 2022ApJ...935..167A) and photutils (Bradley 2023,
astropy/photutils: 1.8.0, Zenodo) in the standard way, i.e. via
subtraction of sky frames and flat field correction. The images were
registered to one another and astrometrically calibrated by matching
stars to the images from Hubble Space Telescope (HST), see below, with
an estimated residual of 0.13" for the seeing-limited images and 0.02"
for the AO images. The Strehl ratio of the AO images were 0.15. The
angular resolution of the seeing-limited and AO images were ∼0.5" and
∼0.09", respectively, derived by determining the Full Width at Half
Maximum (FWHM) of Moffat profiles of isolated sources identified in
each of the images (see Appendix A of Fedriani et al.
2023A&A...676A.107F 2023A&A...676A.107F, for the details).
(2) Pipeline-reduced images from the MAST archive from the Hubble
Space Telescope (HST) of the AFGL 5180 massive star-forming region.
Observations were taken with the HST on the 13th of February, 2016
(program ID: 14465; PI: J. C. Tan). The Wide Field Camera 3 (WFC3)
instrument was used with a pixel scale of 0.13" and FOV of 2'x2'. The
filters F110W (J-band), F128N (Pa-beta), F160W (H-band), and F164N
([FeII]), which have the mean wavelengths 1.180, 1.284, 1.544, and
1.645 microns, and therefore diffraction-limited angular resolutions
of 0.12", 0.13", 0.16", and 0.17", respectively, were employed. The
data was downloaded from the Mikulski Archive for Space Science (MAST)
as a Hubble Advanced Product (HAP), which are reduced and calibrated
using the standard pipeline. The images were astrometrically corrected
by matching stars to the Gaia DR3 catalogue (Gaia Collaboration et al.
2023A&A...674A...1G 2023A&A...674A...1G, Cat. I/350), with an estimated residual of
0.0323", determined by measuring the mean separation between isolated
sources identified using the algorithm DAOFIND (Stetson
1987PASP...99..191S 1987PASP...99..191S) and their Gaia counterparts. The final drizzle
images have a position angle (PA) of 0 degrees.
(3) Reduced continuum images from the Atacama Large
Millimeter/Submillimeter Array (ALMA) of the AFGL 5180 massive
star-forming region, retrieved from the ALMA archive. We used ALMA
1.3mm (Band 6) and 0.9mm (Band 7) continuum data. The ALMA Band 6
observations were carried out on the 23rd of April, 2016 with the
C36-3 configuration, and on the 8th of September, 2016 with the C36-6
configuration (ALMA project ID: 2015.1.01454.S, PI: Y. Zhang). The
total integration times were 3.5 and 6.5 minutes in the two
configurations, respectively. Forty-one antennas were used with
baselines ranging from 15-462m in the C36-3 configuration, and 38
antennas were used with baselines ranging from 15m to 3.2km in the
C36-6 configuration. J0750+1231 and J0510+1800 were used for bandpass
calibration and flux calibration. J0603+2159 was used as a phase
calibrator. The ALMA Band 7 observations were carried out on the 2nd
of December, 2017 using the C43-7 configuration with 48 antennas and
baselines ranging from 41.4m to 6.9km (ALMA project ID:
2017.1.00178.S, PI: T. Hirota). The total integration time was 10
minutes. J0510+1800 was used for bandpass calibration and flux
calibration and J0613+2604 was used as a phase calibrator. The data
were calibrated and imaged in CASA (CASA Team et al.
2022PASP..134.k4502C). After calibration, we performed
self-calibration for each band and configuration using the continuum
data combining the line-free channels. We first performed two
phase-only self-calibration iterations with solution intervals of 30
and 6s, and then one iteration of amplitude self-calibration with the
solution interval equal to the scan intervals. The effective bandwidth
of line-free channels was 1.3GHz and 3.7GHz for the 1.3 and 0.9mm
continuum, respectively. The CASA tclean task was used to image the
data, using Briggs weighting with the robust parameter set to 0.5. The
1.3mm continuum image has a synthetic beam of 0.32"x0.25" and an rms
noise level of 3.1x10-4Jy/beam, and the 0.9mm continuum image has a
synthetic beam of 0.068"x0.067" and rms noise of 1.3x10-4Jy/beam.
Objects:
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RA (2000) DE Designation(s)
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06 08 54.13 +21 38 24.6 AFGL 5180 = GAL 188.95+00.89 = IRAS 06058+2138
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 197 14 List of fits images
fits/* . 14 Individual fits images
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 25 F6.4 arcsec/pix scale ? Scale of the image
27- 30 I4 --- Nx Number of pixels along X-axis
32- 35 I4 --- Ny Number of pixels along Y-axis
37- 62 A26 "datime" Obs.date Observation date
64- 70 F7.3 GHz Freq ? Observed frequency
72- 76 I5 Kibyte size Size of FITS file
78-142 A65 --- FileName Name of FITS file, in subdirectory fits
144-197 A54 --- Title Title of the FITS file
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Acknowledgements:
Samuel Crowe, fec5fg(at)virginia.edu
(End) Patricia Vannier [CDS] 06-Dec-2023