Min Su Yun

SXDF-UDS-CANDELS-ALMA 1.5 arcmin2 deep survey

We have conducted 1.1 mm ALMA observations of a contiguous 105″ × 50″ or 1.5 arcmin2 window (achieved by 19 point mosaic) in the SXDF-UDS-CANDELS. We achieved a 5σ sensitivity of 0.28 mJy, giving a flat sensus of dusty star-forming galaxies with LIR ~6 × 1011 L⊙ (if Tdust = 40 K) or SFR ~100 M⊙ yr-1 up to z~10 thanks to the negative K-correction at this wavelength. We detect 5 brightest sources (S/N>6) and 18 low-significant sources (5 > S/N > 4; they may contain spurious detections, though) in the field. We find that these discrete sources are responsible for a faint filamentary emission seen in low-resolution (~30″) heavily confused AzTEC 1.1mm and SPIRE 0.5mm images. One of the 5 brightest ALMA sources is very dark in deep WFC3 and HAWK-I NIR images as well as VLA 1.4 GHz images, demonstrating that deep ALMA imaging can unveil new obscured star-forming galaxy population.

The VIRUS-P Investigation of the eXtreme Environments of Starbursts (VIXENS): Survey and First Results

Amanda Heiderman∗,1, Neal J. Evans II1, Karl Gebhardt1, Guillermo Blanc2, Timothy A. Davis3, Casey Papovich4, Daisuke Iono5 and Min Yun6 1University of Texas at Austin Department of Astronomy 1 University Station, C1400 Austin, Texas 78712-0259 2Observatories of the Carnegie Institution 813 Santa Barbara Street Pasadena, California 91101 3ESO Karl-Schwarzschild-Strasse 2 D-85748 Garching bei München 4Texas A&M University Department of Physics and Astronomy College Station, TX 77843-4242 5Nobeyama Radio Observatory, NAOJ Minamimaki, Minamisaku, Nagano, 384-1305, Japan 6Department of Astronomy University of Massachusetts Graduate Research Tower B 619E 710 North Pleasant Street Amherst, MA 01003-9305 E-mail: alh@astro.as.utexas.edu

The Large Millimeter telescope Alfonso Serrano: scientific operation of the LMT 50-m, first results and next steps (Conference Presentation)

The Large Millimeter Telescope (LMT) Alfonso Serrano is a bi-national (Mexico and USA) telescope facility operated by the Instituto Nacional de Astrofisica, Optica y Electronica (INAOE) and the University of Massachusetts. The LMT is designed as a 50-m diameter single-dish millimeter-wavelength telescope that is optimized to conduct scientific observations at frequencies between ~70 and 350 GHz. The LMT is constructed on the summit of Sierra Negra at an altitude of 4600m in the Mexican state of Puebla. The site offers excellent mm-wavelength atmospheric transparency all-year round, and the opportunity to conduct submillimeter wavelength observations during the winter months. Following first-light observations in mid-2011, the LMT began regular scientific operations in 2014 with a shared-risk Early Science observing program using the inner 32-m diameter of the primary reflector with an active surface control system. The LMT has already performed successful VLBI observations at 3mm with the High Sensitivity Array and also at 1.3mm as part of the Event Horizon Telescope. Since early 2018 the LMT has begun full scientific operations as a 50-m diameter telescope, making the LMT 50-m the world´s largest single-dish telescope operating at 1.1mm. I will describe the current status of the telescope project, including the early scientific results from the LMT 50-m, as well the instrumentation development program, the plan to improve the overall performance of the telescope, and the on-going transition towards the formation of the LMT Observatory to support the scientific community in their use of the LMT to study the formation and evolution of structure at all cosmic epochs.

What is the origin of a diffuse IGM in compact groups

Since the discovery of large HI deficiencies in Hickson Compa ct Groups (HCGs), the fate of atomic gas in these systems has been a mystery. We previously proposed an evolutionary scenario where the amount of HI decreases with the secular evolu tionary state of a group. But what physical processes give rise to this decrease? Our X-ray stu dy of 8 of the most HI deficient HCGs suggested that galaxy-IGM interaction is not the domin ant mechanism driving cold gas out of group members (Rasmussen et al 2008). In order to explo re this issue further, we have gathered VLA and GBT data for a complete distance-limited sa mple of 22 HCGs with normal, deficient, and highly deficient HI properties. The GBT observ ations (Borthakur et al 2010) revealed evidence for a significant HI excess compared with the interferometer measurements, and this excess appears to increase with the evolutionary phase of th group, possibly associated with the diffusing tidal debris in the IGM. Here, we present the first detailed comparison of VLA & GBT dat a in Stephan’s Quintet (HCG 92) as a first step to examine the spatial and kinematic link be twe n the high surface brightness to diffuse HI emission in these groups. Our preliminary result s suggest that tidal tails could evolve to a diffuse neutral component, as suggested in Verdes-Mont enegro et al (2001) and Borthakur et al (2010).