NOAO >   Observing Info >   Approved Programs >   2017B-0821

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Program Information for 2017B-0821


PI: Matt Berhsady, U. of Wisconsin, Madison, mab@astro.wisc.edu
Address: Astronomy Department, 475 N. Charter St, Madison, WI 53706 USA

CoI: Christy Tremonti, U. of Wisconsin, Madison
CoI: Zachary Pace, U. of Wisconsin, Madison
CoI: Diego Gallegos, U. of Wisconsin, Madison
CoI: Camilo Machuca, U. of Wisconsin, Madison
CoI: Shravan Shetty, U. of Wisconsin, Madison
CoI: Marsha J Wolf, U. of Wisconsin, Madison
CoI: Kate Rubin, San Diego State U.
CoI: Samantha Penny, University of Portsmouth
CoI: Kyle Westfall, UCO / Lick Observatory
CoI: Michele Cappellari, Oxford
CoI: Niv Drory, U. of Texas, Austin
CoI: Renbin Yan, U. of Kentucky
CoI: David Law, STScI
CoI: Kevin Bundy, UCO / Lick Observatory
CoI: Francesco Belfiore, UC Santa Cruz
CoI: Aleks Diamond-Stanic, Bates College

Title: Ground-truth for MaNGA Kinematics: Galactic Winds, ISM Turbulence and Quenched Dwarf Origins

Abstract: Spectroscopic determination of stellar and gas motions -- kinematics -- is a fundamental diagnostic of physical conditions in the interstellar medium and stellar dynamics. In SDSS-IV MaNGA's unsurpassed spectral coverage and sample size is limited by spectral resolution 3-4$times$ larger than the intrinsic line-widths of gas and stars in normal, star- forming spiral disks and dwarf galaxies ($sigmasim$ 20~km/s). The MaNGA survey team have undertaken a major effort to characterize its instrumental resolution. The quality of these corrections appear to be approaching what is required to achieve reliable line-widths at the $sigmasim$30 km/s level for individual emission-lines, but the relaibility for stellar kinematics is less clear; we lack ground-truth, i.e., a reference set of galaxies observed at higher spectral resolution. Given the importance of understanding the fidelity of these corrections for a wide range of science of direct interest to scientists at UW-Madison and across the collaboration, {bf we propose to observe several dozen carefully selected galaxies} from the 10,000 galaxy MaNGA sample over two semesters to calibrate these corrections and establish their accuracy and precision. Galaxies will be observed in the H$alpha$ and H$beta$-MgI regions at instrumental resolutions of 8- 15~km/s. Galaxies will be selected to address compelling science questions concerning the origin of (a) the ubiquitous winds coming from star-forming disks; (b) ISM turbulence; and (c) the quenching of dwarf galaxies.

Program Type: WTAC

Scheduled Nights:
Run 1 (2017B):  WIYN/HEXPK -- 2n on Jan 14 - Jan 15 2018
Run 2 (2017B):  WIYN/HEXPK -- 3n on Jan 18 - Jan 21 2018


National Optical Astronomy Observatory, 950 North Cherry Avenue, P.O. Box 26732, Tucson, Arizona 85726, Phone: (520) 318-8000, Fax: (520) 318-8360



NOAO >   Observing Info >   Approved Programs >   2017B-0821

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