J/ApJ/932/38 A multiwavelength study of GRS 1716-249 in outburst (Saikia+, 2022)
A multiwavelength study of GRS 1716-249 in outburst: constraints on its system
parameters.
Saikia P., Russell D.M., Baglio M.C., Bramich D.M., Casella P.,
Trigo M.D., Gandhi P., Jiang J., Maccarone T., Soria R., Al Noori H.,
Al Yazeedi A., Alabarta K., Belloni T., Bel M.C., Ceccobello C.,
Corbel S., Fender R., Gallo E., Homan J., Koljonen K., Lewis F.,
Markoff S.B., Miller-Jones J.C.A., Rodriguez J., Russell T.D., Shahbaz T.,
Sivakoff G.R., Testa V., Tetarenko A.J.
<Astrophys. J., 932, 38 (2022)>
=2022ApJ...932...38S 2022ApJ...932...38S
ADC_Keywords: Binaries, X-ray; Black holes; Transient; Photometry; Optical;
Photometry, infrared; Radio sources; X-ray sources; Ultraviolet
Keywords: Astrophysical black holes ; Accretion ; Jets ; X-ray binary
stars ; Low-mass x-ray binary stars ; Black hole physics
Abstract:
We present a detailed study of the evolution of the Galactic black
hole transient GRS 1716-249 during its 2016-2017 outburst at optical
(Las Cumbres Observatory), mid-infrared (Very Large Telescope),
near-infrared (Rapid Eye Mount telescope), and ultraviolet (the Neil
Gehrels Swift Observatory Ultraviolet/Optical Telescope) wavelengths,
along with archival radio and X-ray data. We show that the
optical/near-infrared and UV emission of the source mainly originates
from a multi-temperature accretion disk, while the mid-infrared and
radio emission are dominated by synchrotron emission from a compact
jet. The optical/UV flux density is correlated with the X-ray emission
when the source is in the hard state, consistent with an X-ray
irradiated accretion disk with an additional contribution from the
viscous disk during the outburst fade. We find evidence for a weak,
but highly variable jet component at mid-infrared wavelengths. We also
report the long-term optical light curve of the source and find that
the quiescent i'-band magnitude is 21.39 +or- 0.15 mag. Furthermore,
we discuss how previous estimates of the system parameters of the
source are based on various incorrect assumptions, and so are likely
to be inaccurate. By comparing our GRS 1716-249 data set to those of
other outbursting black hole X-ray binaries, we find that while
GRS 1716-249 shows similar X-ray behavior, it is noticeably optically
fainter, if the literature distance of 2.4kpc is adopted. Using
several lines of reasoning, we argue that the source distance is
further than previously assumed in the literature, likely within
4-17kpc, with a most likely range of ∼4-8kpc.
Description:
We monitored GRS 1716-249 during its 2016-2017 outburst extensively
with the Las Cumbres Observatory (LCO) between 2017 January 28 and
October 21 (MJD 57781-58046). Observations were made using the 1m
LCO telescopes at Siding Spring Observatory, Australia, Cerro Tololo
Inter-American Observatory, Chile, and the South African Astronomical
Observatory (SAAO), South Africa, as well as the 2m Faulkes Telescopes
at Haleakala Observatory, Maui, Hawai'i, USA and Siding Spring
Observatory, Australia. The source was also monitored during
quiescence, before and after the 2016-2017 outburst, for 11yr since
2006 February, as part of an ongoing monitoring campaign of
∼50 low-mass X-ray binaries (LMXB) coordinated by the Faulkes
Telescope Project (Lewis+ 2008AIPC.1010..204L 2008AIPC.1010..204L ;
Lewis 2018RTSRE...1..237L 2018RTSRE...1..237L).
Imaging data were primarily taken in the Sloan Digital Sky Survey
(SDSS) g', r', i', and the Panoramic Survey Telescope and Rapid
Response System (Pan-STARRS) Y-band filters, with some data also taken
in Bessel B and V bands.
We detected the source during outburst in a total of 192 images
between 2017 January 28 (MJD 57781) and 2017 October 21 (MJD 58046),
generally at a cadence of every 2-3 days during the brighter phase of
the outburst, and every ∼75s for the high cadence images taken on
2017 May 9 (MJD 57882).
See Section 2.1.1.
We also use the archival data of the source obtained in the G spectral
filter with the Gaia telescope during the recent outburst. Gaia first
detected the source on 2017 January 27 (MJD 57780.8) at G=16.44. Prior
to that, the last observation it had on 29 October 2016 (MJD57690) was
a non-detection (typical detection limit of Gaia is ∼20.7mags,
Brown+ 2016A&A...595A...2G 2016A&A...595A...2G). Gaia detected GRS 1716-249 on 13d during
the outburst, with the last detection on 2017 September 23 (MJD58019).
See Section 2.1.2.
We acquired targeted observations of GRS 1716-249 with the Very Large
Telescope (VLT) in mid-IR wavelengths on three nights during the
2016-2017 outburst, using the VLT Imager and Spectrometer for the
mid-IR (VISIR) instrument on the VLT's UT3 (Melipal). The observations
were made under the programs 098.D-0893 and 099.D-0884 (PI:
D. Russell) in the M band (4.15-5.19um), J8.9 (8.00-9.43um), B10.7
(9.28-12.02um), and PAH2 _2 (11.5-12.3um) filters on 2017 March 25
(MJD 57837), April 21 (MJD 57864), and April 22 (MJD 57865), for
approximately 40-45 minutes total telescope time on each date.
See Section 2.2.1.
We observed GRS 1716-249 in the near-IR wavelengths (J, H, and K
bands, one filter at a time) with the REMIR camera mounted on the
Rapid Eye Mount (REM; La Silla, Chile) telescope between 2017 Feb 8
and October 1 (MJD 57792-58027). See Section 2.2.2.
We also use the archival near-IR photometric observations of
GRS1716-249 during the outburst. See Section 2.2.3.
We gathered publicly available Swift UV/Optical Telescope
(UVOT) pointing observations of the source during its entire outburst
from the NASA/HEASARC data center. See Section 2.3.
We use the radio observations of the source during its outburst with
the Karl G. Jansky Very Large Array (VLA; 5.25, 7.45, 8.8 and
11.0GHz), Australia Telescope Compact Array (ATCA; 5.5 and 9.0GHz) and
Australian Long Baseline Array (LBA; 8.4GHz) as reported in
Bassi+ (2019MNRAS.482.1587B 2019MNRAS.482.1587B) and Atri+ (2019MNRAS.489.3116A 2019MNRAS.489.3116A). Radio
detections of the source are available for 2017 February 9 and 11
(MJD57993 and 57795), April 22 (MJD 57865), August 12 and 13 (MJD57977
and 57978). See Section 2.4.
Finally, we acquired X-ray monitoring data of GRS 1716-249 from the
Swift/BAT and Swift/XRT telescopes. Swift/BAT has observed the source
almost daily from 2016 December 1 (MJD 57723) in the 15-50keV flux
range.
GRS 1716-249 was also observed with Nuclear Spectroscopic Telescope
Array (NuSTAR) during the 2016-2017 outburst.
We also gathered daily X-ray monitoring data of GRS 1716-249 from
MAXI/GSC (Matsuoka+ 2009PASJ...61..999M 2009PASJ...61..999M) in the 2-20keV range covering
the complete outburst.
See Section 2.5.
Objects:
------------------------------------------------------------
RA (2000) DE Designation(s)
------------------------------------------------------------
17 19 36.92 -25 01 04.1 GRS 1716-249 = Granat 1716-249
------------------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 74 142 Faulkes/LCO optical detections of GRS 1716-249
tablea2.dat 81 116 The Rapid Eye Mount (REM) telescope near-IR
detections of GRS 1716-249
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See also:
B/eso : ESO Science Archive Catalog (ESO, 1991-2025)
B/gcvs : General Catalogue of Variable Stars (Samus+, 2007-2017)
V/106 : Catalogue of X-ray binaries (Liu+ 2001)
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
I/358 : Gaia DR3 Part 4. Variability (Gaia Collaboration, 2022)
J/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009)
J/MNRAS/428/2500 : GX 339-4 radio/X-ray flux correlation (Corbel+, 2013)
J/ApJS/209/14 : The Swift/BAT hard X-ray transient monitor (Krimm+, 2013)
J/A+A/587/A61 : BlackCAT BH in Xray transient (Corral-Santana+, 2016)
J/ApJS/222/15 : WATCHDOG: all-sky database of Gal. BHXBs (Tetarenko+, 2016)
J/MNRAS/471/1468 : Transient BH X-ray binaries XMM obs. (Eckersall+, 2017)
J/ApJ/867/105 : ATLAS all-sky stellar ref. cat. ATLAS-REFCAT2 (Tonry+, 2018)
J/A+A/645/A18 : SVOM-ECLAIRs known X-ray sources cat. (Dagoneau+, 2021)
J/ApJ/930/20 : Monitoring of neutron star XRB Centaurus X-4 (Baglio+, 2022)
J/MNRAS/510/4796 : INTEGRAL/IBIS 17-yr X-ray all-sky survey (Krivonos+, 2022)
http://www.sdss.org/ : SDSS home page
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 F11.5 d iMJD [57781.7/58045.8]? Modified Julian Date of
i'-band observation
13- 18 F6.3 mag imag [15.86/18.11]? Apparent i'-band AB magnitude
20- 24 F5.3 mag e_imag [0.003/0.1]? Uncertainty in imag
26- 36 F11.5 d gMJD [57807.3/58045.8]? Modified Julian Date
of g'-band observation
38- 43 F6.3 mag gmag [16.9/19.5]? Apparent g'-band AB magnitude
45- 49 F5.3 mag e_gmag [0.007/0.1]? Uncertainty in gmag
51- 61 F11.5 d rMJD [57790.3/57956.7]? Modified Julian Date
of r'-band observation
63- 68 F6.3 mag rmag [16.36/17.64]? Apparent r'-band AB magnitude
70- 74 F5.3 mag e_rmag [0.005/0.04]? Uncertainty in rmag
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Byte-by-byte Description of file: tablea2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 F11.5 d JMJD [57792.3/58025.1]? Modified Julian Date
of J-band observation
13 A1 --- l_Jmag 3σ upper limit flag on Jmag
when the source was not detected
15- 20 F6.3 mag Jmag [13.16/15.3]? Apparent J-band Vega
magnitude (1)
22- 27 F6.4 mag e_Jmag [0.05/0.3]? Uncertainty in Jmag
29- 39 F11.5 d HMJD [57792.3/58025.1]? Modified Julian Date
of H-band observation
41 A1 --- l_Hmag 3σ upper limit flag on Hmag
when the source was not detected
43- 48 F6.3 mag Hmag [13/15.8]? Apparent H-band Vega
magnitude (1)
50- 54 F5.3 mag e_Hmag [0.06/0.3]? Uncertainty in Hmag
56- 66 F11.5 d KMJD [57792.3/58024.1]? Modified Julian Date
of K-band observation
68 A1 --- l_Kmag 3σ upper limit flag on Kmag
when the source was not detected
70- 75 F6.3 mag Kmag [12.6/14.33]? Apparent K-band Vega
magnitude (1)
77- 81 F5.3 mag e_Kmag [0.09/0.4]? Uncertainty in Kmag
--------------------------------------------------------------------------------
Note (1): The magnitudes are before the subtraction of the contribution from
the nearby star reported here.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Esther Collas [CDS] 17-May-2024