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Autori principali:	O'Brien, Rosalia, Jansen, Rolf A., Grogin, Norman A., Cohen, Seth H., Smith, Brent M., Silver, Ross M., Maksym III, W. P., Windhorst, Rogier A., Carleton, Timothy, Koekemoer, Anton M., Hathi, Nimish P., Willmer, Christopher N. A., Frye, Brenda L., Alpaslan, M., Ashby, M. L. N., Ashcraft, T. A., Bonoli, S., Brisken, W., Cappelluti, N., Civano, F., Conselice, C. J., Dhillon, V. S., Driver, S. P., Duncan, K. J., Dupke, R., Elvis, M., Fazio, G. G., Finkelstein, S. L., Gim, H. B., Griffiths, A., Hammel, H. B., Hyun, M., Im, M., Jones, V. R., Kim, D., Ladjelate, B., Larson, R. L., Malhotra, S., Marshall, M. A., Milam, S. N., Pierel, J. D. R., Rhoads, J. E., Rodney, S. A., Röttgering, H. J. A., Rutkowski, M. J., Ryan, Jr., R. E., Ward, M. J., White, C. W., van Weeren, R. J., Zhao, X., Summers, J., D'Silva, J. C. J., Ortiz III, R., Robotham, A. S. G., Coe, D., Nonino, M., Pirzkal, N., Yan, H., Acharya, T.
Natura:	Preprint
Pubblicazione:	2024
Soggetti:	Astrophysics of Galaxies
Accesso online:	https://arxiv.org/abs/2401.04944
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_version_	1866929334448553984
author	O'Brien, Rosalia Jansen, Rolf A. Grogin, Norman A. Cohen, Seth H. Smith, Brent M. Silver, Ross M. Maksym III, W. P. Windhorst, Rogier A. Carleton, Timothy Koekemoer, Anton M. Hathi, Nimish P. Willmer, Christopher N. A. Frye, Brenda L. Alpaslan, M. Ashby, M. L. N. Ashcraft, T. A. Bonoli, S. Brisken, W. Cappelluti, N. Civano, F. Conselice, C. J. Dhillon, V. S. Driver, S. P. Duncan, K. J. Dupke, R. Elvis, M. Fazio, G. G. Finkelstein, S. L. Gim, H. B. Griffiths, A. Hammel, H. B. Hyun, M. Im, M. Jones, V. R. Kim, D. Ladjelate, B. Larson, R. L. Malhotra, S. Marshall, M. A. Milam, S. N. Pierel, J. D. R. Rhoads, J. E. Rodney, S. A. Röttgering, H. J. A. Rutkowski, M. J. Ryan, Jr., R. E. Ward, M. J. White, C. W. van Weeren, R. J. Zhao, X. Summers, J. D'Silva, J. C. J. Ortiz III, R. Robotham, A. S. G. Coe, D. Nonino, M. Pirzkal, N. Yan, H. Acharya, T.
author_facet	O'Brien, Rosalia Jansen, Rolf A. Grogin, Norman A. Cohen, Seth H. Smith, Brent M. Silver, Ross M. Maksym III, W. P. Windhorst, Rogier A. Carleton, Timothy Koekemoer, Anton M. Hathi, Nimish P. Willmer, Christopher N. A. Frye, Brenda L. Alpaslan, M. Ashby, M. L. N. Ashcraft, T. A. Bonoli, S. Brisken, W. Cappelluti, N. Civano, F. Conselice, C. J. Dhillon, V. S. Driver, S. P. Duncan, K. J. Dupke, R. Elvis, M. Fazio, G. G. Finkelstein, S. L. Gim, H. B. Griffiths, A. Hammel, H. B. Hyun, M. Im, M. Jones, V. R. Kim, D. Ladjelate, B. Larson, R. L. Malhotra, S. Marshall, M. A. Milam, S. N. Pierel, J. D. R. Rhoads, J. E. Rodney, S. A. Röttgering, H. J. A. Rutkowski, M. J. Ryan, Jr., R. E. Ward, M. J. White, C. W. van Weeren, R. J. Zhao, X. Summers, J. D'Silva, J. C. J. Ortiz III, R. Robotham, A. S. G. Coe, D. Nonino, M. Pirzkal, N. Yan, H. Acharya, T.
contents	The JWST North Ecliptic Pole (NEP) Time Domain Field (TDF) is a $>$14 arcmin diameter field optimized for multi-wavelength time-domain science with JWST. It has been observed across the electromagnetic spectrum both from the ground and from space, including with the Hubble Space Telescope (HST). As part of HST observations over 3 cycles (the "TREASUREHUNT" program), deep images were obtained with ACS/WFC in F435W and F606W that cover almost the entire JWST NEP TDF. Many of the individual pointings of these programs partially overlap, allowing an initial assessment of the potential of this field for time-domain science with HST and JWST. The cumulative area of overlapping pointings is ~88 arcmin$^2$, with time intervals between individual epochs that range between 1 day and 4$+$ years. To a depth of $m_{AB}$ $\simeq$ 29.5 mag (F606W), we present the discovery of 12 transients and 190 variable candidates. For the variable candidates, we demonstrate that Gaussian statistics are applicable, and estimate that ~80 are false positives. The majority of the transients will be supernovae, although at least two are likely quasars. Most variable candidates are AGN, where we find 0.42% of the general $z$ $<$ 6 field galaxy population to vary at the $~3σ$ level. Based on a 5-year timeframe, this translates into a random supernova areal density of up to ~0.07 transients per arcmin$^2$ (~245 deg$^{-2}$) per epoch, and a variable AGN areal density of ~1.25 variables per arcmin$^2$ (~4500 deg$^{-2}$) to these depths.
format	Preprint
id	arxiv_https___arxiv_org_abs_2401_04944
institution	arXiv
publishDate	2024
record_format	arxiv
spellingShingle	TREASUREHUNT: Transients and Variability Discovered with HST in the JWST North Ecliptic Pole Time Domain Field O'Brien, Rosalia Jansen, Rolf A. Grogin, Norman A. Cohen, Seth H. Smith, Brent M. Silver, Ross M. Maksym III, W. P. Windhorst, Rogier A. Carleton, Timothy Koekemoer, Anton M. Hathi, Nimish P. Willmer, Christopher N. A. Frye, Brenda L. Alpaslan, M. Ashby, M. L. N. Ashcraft, T. A. Bonoli, S. Brisken, W. Cappelluti, N. Civano, F. Conselice, C. J. Dhillon, V. S. Driver, S. P. Duncan, K. J. Dupke, R. Elvis, M. Fazio, G. G. Finkelstein, S. L. Gim, H. B. Griffiths, A. Hammel, H. B. Hyun, M. Im, M. Jones, V. R. Kim, D. Ladjelate, B. Larson, R. L. Malhotra, S. Marshall, M. A. Milam, S. N. Pierel, J. D. R. Rhoads, J. E. Rodney, S. A. Röttgering, H. J. A. Rutkowski, M. J. Ryan, Jr., R. E. Ward, M. J. White, C. W. van Weeren, R. J. Zhao, X. Summers, J. D'Silva, J. C. J. Ortiz III, R. Robotham, A. S. G. Coe, D. Nonino, M. Pirzkal, N. Yan, H. Acharya, T. Astrophysics of Galaxies The JWST North Ecliptic Pole (NEP) Time Domain Field (TDF) is a $>$14 arcmin diameter field optimized for multi-wavelength time-domain science with JWST. It has been observed across the electromagnetic spectrum both from the ground and from space, including with the Hubble Space Telescope (HST). As part of HST observations over 3 cycles (the "TREASUREHUNT" program), deep images were obtained with ACS/WFC in F435W and F606W that cover almost the entire JWST NEP TDF. Many of the individual pointings of these programs partially overlap, allowing an initial assessment of the potential of this field for time-domain science with HST and JWST. The cumulative area of overlapping pointings is ~88 arcmin$^2$, with time intervals between individual epochs that range between 1 day and 4$+$ years. To a depth of $m_{AB}$ $\simeq$ 29.5 mag (F606W), we present the discovery of 12 transients and 190 variable candidates. For the variable candidates, we demonstrate that Gaussian statistics are applicable, and estimate that ~80 are false positives. The majority of the transients will be supernovae, although at least two are likely quasars. Most variable candidates are AGN, where we find 0.42% of the general $z$ $<$ 6 field galaxy population to vary at the $~3σ$ level. Based on a 5-year timeframe, this translates into a random supernova areal density of up to ~0.07 transients per arcmin$^2$ (~245 deg$^{-2}$) per epoch, and a variable AGN areal density of ~1.25 variables per arcmin$^2$ (~4500 deg$^{-2}$) to these depths.
title	TREASUREHUNT: Transients and Variability Discovered with HST in the JWST North Ecliptic Pole Time Domain Field
topic	Astrophysics of Galaxies
url	https://arxiv.org/abs/2401.04944

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