ADS
arXiv
I assisted in many of the technical aspects of the paper including Bolocam and VLA data reduction.
We identify a potential evolutionary sequence among millimeter "clumps". HCO+ and N2H+ maps are used to measure the physical properties of some of these clumps.
Monday, July 11, 2011
Star-forming Region Sh 2-233IR. I. Deep Near-infrared Observations toward the Embedded Stellar Clusters
The Bolocam Galactic Plane Survey IV: λ = 1.1 and 0.35 mm Dust Continuum Emission in the Galactic Center Region
The Bolocam Galactic Plane Survey. III. Characterizing Physical Properties of Massive Star-forming Regions in the Gemini OB1 Molecular Cloud
ADS
arXiv
As with the other Bolocam papers, I reduced the data. All of the analysis work was done by Miranda.
Because of Gem OB1's known distance (~2 kpc), it was possible to derive the physical properties of all of the 34 BGPS sources. NH3 temperatures and line widths were combined to measure total dust mass, density, and virial parameter. This paper is the best characterization of "typical" BGPS sources, at least for the outer galaxy.
arXiv
As with the other Bolocam papers, I reduced the data. All of the analysis work was done by Miranda.
Because of Gem OB1's known distance (~2 kpc), it was possible to derive the physical properties of all of the 34 BGPS sources. NH3 temperatures and line widths were combined to measure total dust mass, density, and virial parameter. This paper is the best characterization of "typical" BGPS sources, at least for the outer galaxy.
The Bolocam Galactic Plane Survey. II. Catalog of the Image Data
ADS
arXiv
My primary contribution to this work was reducing the data from which catalogs were derived. As part of this process, I also made the noise maps that were part of the Bolocat process and did some of the by-eye verification work.
Bolocat extracted >8000 sources from the BGPS using a watershed decomposition method. Most of these sources have now been observed with the HHT in HCO+ and N2H+ to determine their velocity and kinematic distance.
arXiv
My primary contribution to this work was reducing the data from which catalogs were derived. As part of this process, I also made the noise maps that were part of the Bolocat process and did some of the by-eye verification work.
Bolocat extracted >8000 sources from the BGPS using a watershed decomposition method. Most of these sources have now been observed with the HHT in HCO+ and N2H+ to determine their velocity and kinematic distance.
The Bolocam Galactic Plane Survey: Survey Description and Data Reduction
ADS
arXiv
I wrote about half of this paper and did the majority of the work described, including writing the data pipeline and reducing all of the data. However, there was a good deal of work done on the project before I showed up on the scene.
The paper describes the methods by which we reduced the Bolocam observations of the Northern Galactic Plane and the tests we ran to determine how well we recovered the "true" sky structure.
arXiv
I wrote about half of this paper and did the majority of the work described, including writing the data pipeline and reducing all of the data. However, there was a good deal of work done on the project before I showed up on the scene.
The paper describes the methods by which we reduced the Bolocam observations of the Northern Galactic Plane and the tests we ran to determine how well we recovered the "true" sky structure.
Outflows and Massive Stars in the protocluster IRAS 05358+3543
ADS
arXiv
A mm and near-IR study of the IRAS 05358+3543 system. Recently (2011), it has become clear that "protocluster" is unlikely to be the right label for IRAS 05358+3543. "proto-association" might be more accurate.
Perhaps the most interesting result of this paper is the discovery that the central source is likely to be a 400-AU binary with two massive (>8 msun) stars at different evolutionary stages. It is just barely in ALMA's range...
arXiv
A mm and near-IR study of the IRAS 05358+3543 system. Recently (2011), it has become clear that "protocluster" is unlikely to be the right label for IRAS 05358+3543. "proto-association" might be more accurate.
Perhaps the most interesting result of this paper is the discovery that the central source is likely to be a 400-AU binary with two massive (>8 msun) stars at different evolutionary stages. It is just barely in ALMA's range...
A spatially resolved study of photoelectric heating and [C II] cooling in the LMC. Comparison with dust emission as seen by SAGE
Kinematics and H2 morphology of the multipolar post-AGB star IRAS 16594-4656
ADS
arXiv
An interesting examination of the morphology of the circumstellar material around IRAS 16594-4656. I did this work with Toshiya Ueta at the University of Denver. My contribution was azimuthally interpolating the 7 high-resolution long-slit spectra onto a 3-dimensional grid, creating a full 3D position-velocity cube. I used the Perl Data Language, which I have since abandoned.
arXiv
An interesting examination of the morphology of the circumstellar material around IRAS 16594-4656. I did this work with Toshiya Ueta at the University of Denver. My contribution was azimuthally interpolating the 7 high-resolution long-slit spectra onto a 3-dimensional grid, creating a full 3D position-velocity cube. I used the Perl Data Language, which I have since abandoned.
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