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Vol. 58 (2024), Contributions
Vol. 58 (2024)
Contributions

The DECam Magellanic Clouds Emission-Line Surveys

DOI: https://doi.org/10.22201/ia.14052059p.2024.58.15
S. D. Points
NSF's NOIRLab, CTIO, Casilla 603, La Serena, Chile.
K. S. Long
Space Telescope Science Institute, 3700 San Martin Dr, Baltimore MD, 21218, USA. & Eureka Scientific, Inc.,2452 Delmer Street, Suite 100, Oakland, CA 94602-3017, USA.
W. P. Blair
The William H. Miller III Department of Physics and Astronomy, Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD, 21218, USA.
P. F. Winkler
Department of Physics, Middlebury College, Middlebury, VT, 05753, USA.
R. M. Williams
Department of Earth and Space Sciences, Columbus State University, 4225 University Avenue, Columbus, Georgia 31907, USA.
Y. -H. Chu
Academia Sinica, 11F of AS/NTU Astronomy-Mathematics Building, No.1, Sec. 4, Roosevelt Rd, Taipei 10617, Taiwan, R.O.C.
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Keywords

H II regions
ISM: supernova remnants
Magellanic Clouds

How to Cite

The DECam Magellanic Clouds Emission-Line Surveys. (2024). Revista Mexicana De Astrofísica Y Astronomía Serie De Conferencias, 58, 45-47. https://doi.org/10.22201/ia.14052059p.2024.58.15
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Abstract

We have used the Dark Energy Camera (DECam) on the CTIO Blanco 4-m telescope to perform a new emission-line survey of the Large and Small Magellanic Clouds (LMC and SMC, respectively) with unprecedented spatial resolution, using narrow-band Hα and [S ii] filters in addition to a continuum band for use in subtraction. These data are comparable in depth to extant emission-line surveys of the Magellanic Clouds (e.g., MCELS), but with higher angular resolution. We have created a custom Python-based pipeline to reduce these data and present examples of our first results.

Resumen

Hemos utilizado la Cámara de Energía Oscura (DECam) en el telescopio CTIO Blanco de 4 metros para realizar un nuevo estudio de líneas de emisión de las Nubes Grande y Pequeña de Magallanes (LMC y SMC, respectivamente) con una resolución espacial sin precedentes, utilizando filtros Hα de banda estrecha y [S,ii], además de una banda de continuo para sustracción. Estos datos son comparables en profundidad a los estudios de líneas de emisión existentes de las Nubes de Magallanes (por ejemplo, MCELS), pero con una mayor resolución angular. Hemos creado una pipeline personalizada basada en Python para reducir estos datos y presentar ejemplos de nuestros primeros resultados.

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