Eric Koch

The 2013 outburst of a transient very faint X-ray binary, 23 arcsec from Sgr A*

We report observations using the Swift/XRT, NuSTAR, and Chandra X-ray telescopes of the transientX-raysourceCXOGCJ174540.0-290005duringits2013outburst.Duetoitslocation in the field of multiple observing campaigns targeting Sgr A*, this is one of the best-studied outbursts of a very faint X-ray binary (VFXB; peak LX < 10 36 erg s −1 ) yet recorded, with detections in 173 ks of X-ray observations over 50 d. VFXBs are of particular interest, due to their unusually low outburst luminosities and time-averaged mass transfer rates, which are hard to explain within standard accretion physics and binary evolution. The 2013 outburst of CXOGC J174540.0-290005 peaked at LX(2–10 keV) = 5.0 × 10 35 erg s −1 , and all data above 10 34 erg s −1 were well fitted by an absorbed power law of photon index ∼1.7, extending from 2 keV out to 70 keV. We discuss the implications of these observations for the accretion state of CXOGC J174540.0-290005.

AN EXPLORATION OF THE STATISTICAL SIGNATURES OF STELLAR FEEDBACK

All molecular clouds are observed to be turbulent, but the origin, means of sustenance, and evolution of the turbulence remain debated. One possibility is that stellar feedback injects enough energy into the cloud to drive observed motions on parsec scales. Recent numerical studies of molecular clouds have found that feedback from stars, such as protostellar outflows and winds, injects energy and impacts turbulence. We expand upon these studies by analyzing magnetohydrodynamic simulations of molecular clouds, including stellar winds, with a range of stellar mass-loss rates and magnetic field strengths. We generate synthetic

Assessing the Impact of Astrochemistry on Molecular Cloud Turbulence Statistics

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Kinematics of the Atomic ISM in M33 on 80 pc scales

CO(1-0) maps assuming that the simulations are at the distance of the nearby Perseus molecular cloud. By comparing the outputs from different initial conditions and evolutionary times, we identify differences in the synthetic observations and characterize these using common astrostatistics. We quantify the different statistical responses using a variety of metrics proposed in the literature. We find that multiple astrostatistics, including principal component analysis, the spectral correlation function and the velocity coordinate spectrum, are sensitive to changes in stellar mass-loss rates and/or time evolution. A few statistics, including the Cramer statistic and velocity coordinate spectrum, are sensitive to the magnetic field strength. These findings demonstrate that stellar feedback influences molecular cloud turbulence and can be identified and quantified observationally using such statistics.

Cloud Structure of Galactic OB Cluster Forming Regions from Combining Ground and Space Based Bolometric Observations

We analyze hydrodynamic simulations of turbulent, star-forming molecular clouds that are post-processed with the photo-dissociation region astrochemistry code 3D-PDR. We investigate the sensitivity of 15 commonly applied turbulence statistics to post-processing assumptions, namely variations in gas temperature, abundance and external radiation field. We produce synthetic

Cloud structure of three Galactic infrared dark star-forming regions from combining ground and space based bolometric observations

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Detection of an OH 1665 MHz Maser in M33

CO(1-0) and CI(

radio-astro-tools/spectral-cube: v0.4.3 release

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Erratum: Kinematics of the Atomic ISM in M33 on 80 pc scales

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Erratum: “Cloud Structure of Three Galactic Infrared Dark Star-forming Regions from Combining Ground and Space-based Bolometric Observations” (2017, ApJ, 840, 22)

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