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.
Articles by Adam (keflavich@gmail.com)
Herschel observations of the W43 "mini-starburst"
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.
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.
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.
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.
Galactic Center Photo Contest
The Galactic Center and the surrounding Central Molecular Zone comprise the most active star formation region in the Milky Way. This 2 x 1 degree field was imaged at 20 cm (purple) with the NRAO Very Large Array, tracing H II regions that are illuminated by hot, massive stars, supernova remnants, and synchrotron emission. Emission at 1.1 mm (orange) was observed with the Caltech Submillimeter Observatory and highlights cold (20-30 K) dust associated with molecular gas. Some of this material will form stars within in the next few million years; the remainder will be blown away. The diffuse cyan and colored star images are from the Spitzer Space Observatory's Infrared Array Camera. The cyan is primarily emission from stars, the point sources, and from polycyclic aromatic hydrocarbons (PAHs), the diffuse component.
My view of the Galactic Center is the winner of this year's NRAO photo contest. It displays a multiwavelength view of the galactic center. The caption at the NRAO photo contest (reproduced above) describes it well, but I will go into further depth here.
The 'arches' are the large purple filamentary structures seen near the brightest point in the map, Sgr A*, the center of our galaxy. They are thought to be large scale magnetic fields possibly generated by winds from hot stars. Farhad Yusef-Zadeh, my collaborator on the photo, leads the study of radio emission from the Galactic Center. The orange color is 1.1mm emission, which means that we're seeing something completely different. This light actually comes from dust. We usually see dust in absorption because in the optical, it blocks light. There is so much dust between us and the Galactic Center that we can't see it at all at optical wavelengths.
Sagittarius B2 is the bright blob just to the left of center. It is the most massive collection of gas and dust in our galaxy. It is full of different types of molecules including complex organic molecules. A new generation of massive stars is thought to be forming there. Spitzer's 8 micron view is presented in cyan. Mostly this comes from PAH, Polycyclic Aromatic Hydrocarbon, emission. PAHs are big molecules with lots of Carbon and Hydrogen chained together. Stars are visible at these wavelengths because the dust isn't as effective at blocking out infrared light - but look closely at the orange regions on the right side of the image. You might notice that not only is there dust there, but there's also less PAH emission visible. This is because on the right side of the Galactic Center, the spiral arm is behind the dust, and on the left side it is in front. When dust blocks out infrared light, the object we see is called an 'infrared dark cloud'. These clouds are usually places where star formation has not yet started, but will soon. This image was created using GIMP, the Gnu Image Manipulation Program, using a variety of layers, opacities, etc.
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