TY - JOUR
T1 - The AstroSat UV Deep Field North
T2 - The Far- and Near-ultraviolet Photometric Catalog
AU - Mondal, Chayan
AU - Saha, Kanak
AU - Bhattacharya, Souradeep
AU - Borgohain, Anshuman
AU - Tandon, Shyam N.
AU - Rafelski, Marc
AU - Jansen, Rolf A.
AU - Windhorst, Rogier A.
AU - Teplitz, Harry I.
AU - Smith, Brent M.
N1 - Funding Information:
This work is primarily based on observations taken by AstroSat/UVIT. The UVIT project is a result of collaboration between the Indian Institute of Astrophysics, Bengaluru, Inter‐University Centre for Astronomy and Astrophysics, Pune, Tata Institute of Fundamental Research, Mumbai, several centers of ISRO, and the Canadian Space Agency. Indian Institutions and the Canadian Space Agency have contributed to the work presented in this paper. Several groups from ISAC (ISRO), Bengaluru, and IISU (ISRO), and Trivandrum have contributed to the design, fabrication, and testing of the payload. The Mission Group (ISAC) and ISTRAC (ISAC) continue to provide support by making observations with, and reception and initial processing of the data. R.A.W. and R.A.J. acknowledge support from NASA JWST Interdisciplinary Scientist grants NAG5-12460, NNX14AN10G, and 80NSSC18K0200 from GSFC. We gratefully thank all the individuals involved in the various teams for providing their support to the project from the early stages of the design to launch and observations with it in the orbit. We acknowledge support from HST grants HST-GO-15647, and we used observations taken by the CANDELS survey (HST-GO-9425 and HST-GO-9583) with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This research made use of Matplotlib (Hunter ), Astropy (Astropy Collaboration et al. , ), photutils (Bradley et al. ) community-developed core Python packages for Astronomy and SAOImageDS9 (Joye & Mandel ). Finally, we thank the referee for valuable suggestions.
Funding Information:
This work is primarily based on observations taken by AstroSat/UVIT. The UVIT project is a result of collaboration between the Indian Institute of Astrophysics, Bengaluru, Inter‐University Centre for Astronomy and Astrophysics, Pune, Tata Institute of Fundamental Research, Mumbai, several centers of ISRO, and the Canadian Space Agency. Indian Institutions and the Canadian Space Agency have contributed to the work presented in this paper. Several groups from ISAC (ISRO), Bengaluru, and IISU (ISRO), and Trivandrum have contributed to the design, fabrication, and testing of the payload. The Mission Group (ISAC) and ISTRAC (ISAC) continue to provide support by making observations with, and reception and initial processing of the data. R.A.W. and R.A.J. acknowledge support from NASA JWST Interdisciplinary Scientist grants NAG5-12460, NNX14AN10G, and 80NSSC18K0200 from GSFC. We gratefully thank all the individuals involved in the various teams for providing their support to the project from the early stages of the design to launch and observations with it in the orbit. We acknowledge support from HST grants HST-GO-15647, and we used observations taken by the CANDELS survey (HST-GO-9425 and HST-GO-9583) with the NASA/ESA Hubble Space Telescope, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This research made use of Matplotlib (Hunter 2007), Astropy (Astropy Collaboration et al. 2013, 2018), photutils (Bradley et al. 2020) community-developed core Python packages for Astronomy and SAOImageDS9 (Joye & Mandel 2003). Finally, we thank the referee for valuable suggestions.
Publisher Copyright:
© 2023. The Author(s). Published by the American Astronomical Society.
PY - 2023/2/1
Y1 - 2023/2/1
N2 - We present deep UV imaging observations of the Great Observatories Origins Survey Northern (GOODS-N) field with AstroSat/UVIT (AstroSat UV Deep Field north—AUDFn), using one far-UV (FUV) (F154W, 34.0 ks) and two near-UV (NUV) filters (N242W, 19.2 ks; N245M, 15.5 ks). The nature of the UV sky background was explored across the UVIT field, and a global mean and rms were estimated for each filter. We reach 3σ detection limits of m AB ∼ 27.35, 27.28, and 27.02 mag for a point source in the F154W, N242W, and N245M bands respectively. The 50% completeness limits of the FUV and NUV images are m AB = 26.40 and 27.05 mag respectively. We constructed point-spread functions for each band and estimated their FWHM, which were found to be almost the same: 1.″18 in F154W, 1.″11 in N242W, and 1.″24 in N245M. We used SExtractor to separately identify sources in the FUV and NUV filters and produce the UV source catalog of the entire AUDFn field. The source count slope estimated in FUV and NUV is 0.57 dex mag−1 (between 19 and 25 mag) and 0.44 dex mag−1 (between 18 and 25 mag), respectively. The catalog contains 6839 and 16,171 sources (brighter than the 50% completeness limit) in the FUV and NUV, respectively. Our FUV and NUV flux measurements of the identified sources complement existing multiband data in the GOODS-N field, and enable us to probe rest-frame FUV properties of galaxies at redshift z < 1 and search for candidate Lyman continuum leakers at redshift z > 0.97.
AB - We present deep UV imaging observations of the Great Observatories Origins Survey Northern (GOODS-N) field with AstroSat/UVIT (AstroSat UV Deep Field north—AUDFn), using one far-UV (FUV) (F154W, 34.0 ks) and two near-UV (NUV) filters (N242W, 19.2 ks; N245M, 15.5 ks). The nature of the UV sky background was explored across the UVIT field, and a global mean and rms were estimated for each filter. We reach 3σ detection limits of m AB ∼ 27.35, 27.28, and 27.02 mag for a point source in the F154W, N242W, and N245M bands respectively. The 50% completeness limits of the FUV and NUV images are m AB = 26.40 and 27.05 mag respectively. We constructed point-spread functions for each band and estimated their FWHM, which were found to be almost the same: 1.″18 in F154W, 1.″11 in N242W, and 1.″24 in N245M. We used SExtractor to separately identify sources in the FUV and NUV filters and produce the UV source catalog of the entire AUDFn field. The source count slope estimated in FUV and NUV is 0.57 dex mag−1 (between 19 and 25 mag) and 0.44 dex mag−1 (between 18 and 25 mag), respectively. The catalog contains 6839 and 16,171 sources (brighter than the 50% completeness limit) in the FUV and NUV, respectively. Our FUV and NUV flux measurements of the identified sources complement existing multiband data in the GOODS-N field, and enable us to probe rest-frame FUV properties of galaxies at redshift z < 1 and search for candidate Lyman continuum leakers at redshift z > 0.97.
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U2 - 10.3847/1538-4365/aca7c4
DO - 10.3847/1538-4365/aca7c4
M3 - Article
AN - SCOPUS:85147447368
SN - 0067-0049
VL - 264
JO - Astrophysical Journal, Supplement Series
JF - Astrophysical Journal, Supplement Series
IS - 2
M1 - 40
ER -