Jet-ISM Interactions near the Microquasars GRS 1758-258 and 1E 1740.7-2942. (arXiv:2007.11085v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Tetarenko_A/0/1/0/all/0/1">A.J. Tetarenko</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosolowsky_E/0/1/0/all/0/1">E.W. Rosolowsky</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_Jones_J/0/1/0/all/0/1">J.C.A Miller-Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sivakoff_G/0/1/0/all/0/1">G.R. Sivakoff</a>
We present Atacama Large Millimeter/Sub-millimeter Array observations of the
candidate jet-ISM interaction zones near the black hole X-ray binaries GRS
1758$-$258 and 1E 1740.7$-$2942. Using these data, we map the molecular line
emission in the regions, detecting emission from the HCN [$J=1-0$], HCO$^+$
[$J=1-0$], SiO [$J=2-1$], CS [$J=2-1$], $^{13}$CO [$J=1-0$], C$^{18}$O
[$J=1-0$], HNCO [$J=4_{0,4}-3_{0,3}$], HNCO [$J=5_{0,5}-4_{0,4}$], and CH$_3$OH
[$J=2_{1,1}-1_{1,0}$] molecular transitions. Through examining the
morphological, spectral, and kinematic properties of this emission, we identify
molecular structures that may trace jet-driven cavities in the gas surrounding
these systems. Our results from the GRS 1758$-$258 region in particular, are
consistent with recent work, which postulated the presence of a jet-blown
cocoon structure in deep radio continuum maps of the region. Using these newly
discovered molecular structures as calorimeters, we estimate the time averaged
jet power from these systems, finding $(1.1-5.7)times10^{36}{rm erg,s}^{-1}$
over $0.12-0.31$ Myr for GRS 1758$-$258 and $(0.7-3.5)times10^{37}{rm
erg,s}^{-1}$ over $0.10-0.26$ Myr for 1E 1740.7$-$2942. Additionally, the
spectral line characteristics of the detected emission place these molecular
structures in the central molecular zone of our Galaxy, thereby constraining
the distances to the black hole X-ray binaries to be $8.0pm1.0$ kpc. Overall,
our analysis solidifies the diagnostic capacity of molecular lines, and
highlights how astro-chemistry can both identify jet-ISM interaction zones and
probe jet feedback from Galactic X-ray binaries.
We present Atacama Large Millimeter/Sub-millimeter Array observations of the
candidate jet-ISM interaction zones near the black hole X-ray binaries GRS
1758$-$258 and 1E 1740.7$-$2942. Using these data, we map the molecular line
emission in the regions, detecting emission from the HCN [$J=1-0$], HCO$^+$
[$J=1-0$], SiO [$J=2-1$], CS [$J=2-1$], $^{13}$CO [$J=1-0$], C$^{18}$O
[$J=1-0$], HNCO [$J=4_{0,4}-3_{0,3}$], HNCO [$J=5_{0,5}-4_{0,4}$], and CH$_3$OH
[$J=2_{1,1}-1_{1,0}$] molecular transitions. Through examining the
morphological, spectral, and kinematic properties of this emission, we identify
molecular structures that may trace jet-driven cavities in the gas surrounding
these systems. Our results from the GRS 1758$-$258 region in particular, are
consistent with recent work, which postulated the presence of a jet-blown
cocoon structure in deep radio continuum maps of the region. Using these newly
discovered molecular structures as calorimeters, we estimate the time averaged
jet power from these systems, finding $(1.1-5.7)times10^{36}{rm erg,s}^{-1}$
over $0.12-0.31$ Myr for GRS 1758$-$258 and $(0.7-3.5)times10^{37}{rm
erg,s}^{-1}$ over $0.10-0.26$ Myr for 1E 1740.7$-$2942. Additionally, the
spectral line characteristics of the detected emission place these molecular
structures in the central molecular zone of our Galaxy, thereby constraining
the distances to the black hole X-ray binaries to be $8.0pm1.0$ kpc. Overall,
our analysis solidifies the diagnostic capacity of molecular lines, and
highlights how astro-chemistry can both identify jet-ISM interaction zones and
probe jet feedback from Galactic X-ray binaries.
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