Multiwavelength Surveys within the DEEP Fields

The Pan-STARRS1 survey is collecting multi-epoch, multi-colour observations of the sky north of declination −30 ° , and has designated 70 deg 2 for nightly observations that are particularly useful for transient detection. A duplicate, Pan-STARRS2, is nearing completion that offers opportunities to improve the quality of transient search and observation, as well as simply increasing the number of detections. A new system, the Asteroid Terrestrial-impact Last Alert System (ATLAS), increases the search area to all-sky in return for diminished sensitivity, and highlights tension among optimization for static sky images, optimization for faint transients and optimization for an unbiased number of transients. ATLAS gives up sub-arcsecond images and full colour information to specialize in the third category, but should detect many more transients than the Pan-STARRS1 Medium Deep fields or the Palomar Transient Factory, with examples of transient classes that are considerably closer and brighter.

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You Can Almost See Forever: The Hubble Deep Fields

Life With Hubble ◽

10.1088/2514-3433/ab8ad0ch11 ◽

2020 ◽

Author(s):

David S Leckrone

Keyword(s):

Hubble Deep Fields ◽

Deep Fields

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HST/ACS OBSERVATIONS OF RR LYRAE STARS IN SIX ULTRA-DEEP FIELDS OF M31

The Astronomical Journal ◽

10.1088/0004-6256/141/5/171 ◽

2011 ◽

Vol 141 (5) ◽

pp. 171 ◽

Cited By ~ 26

Author(s):

E. J. Jeffery ◽

E. Smith ◽

T. M. Brown ◽

A. V. Sweigart ◽

J. S. Kalirai ◽

...

Keyword(s):

Rr Lyrae Stars ◽

Rr Lyrae ◽

Deep Fields ◽

Lyrae Stars

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Hubble Sequence as a Temporal Evolution Sequence

Symposium - International Astronomical Union ◽

10.1017/s0074180900113555 ◽

1999 ◽

Vol 186 ◽

pp. 491-491

Author(s):

Xiaolei Zhang

Keyword(s):

Spiral Galaxies ◽

Temporal Evolution ◽

Natural Question ◽

Late Type ◽

Present Epoch ◽

Hubble Sequence ◽

Deep Survey ◽

Deep Fields ◽

The Universe ◽

Evolution Sequence

The results from Hubble Space Telescope's Medium Deep Survey and Deep Fields indicate that there exists far more blue spiral galaxies at the intermediate and high redshifts than at the present epoch. A natural question therefore is: what have become of these excess late type galaxies as the Universe aged?

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The deep Chandra survey in the SDSS J1030+0524 field

Astronomy and Astrophysics ◽

10.1051/0004-6361/202037914 ◽

2020 ◽

Vol 637 ◽

pp. A52 ◽

Cited By ~ 2

Author(s):

R. Nanni ◽

R. Gilli ◽

C. Vignali ◽

M. Mignoli ◽

A. Peca ◽

...

Keyword(s):

Large Scale ◽

Near Infrared ◽

Infrared Imaging ◽

Cumulative Number ◽

Imaging Data ◽

X Ray ◽

Large Scale Structures ◽

Multi Wavelength ◽

Deep Fields ◽

Initial Source

We present the X-ray source catalog for the ∼479 ks Chandra exposure of the SDSS J1030+0524 field, which is centered on a region that shows the best evidence to date of an overdensity around a z > 6 quasar, and also includes a galaxy overdensity around a Compton-thick Fanaroff-Riley type II (FRII) radio galaxy at z = 1.7. Using wavdetect for initial source detection and ACIS Extract for source photometry and significance assessment, we create preliminary catalogs of sources that are detected in the full (0.5−7.0 keV), soft (0.5−2.0 keV), and hard (2−7 keV) bands, respectively. We produce X-ray simulations that mirror our Chandra observation to filter our preliminary catalogs and achieve a completeness level of > 91% and a reliability level of ∼95% in each band. The catalogs in the three bands are then matched into a final main catalog of 256 unique sources. Among them, 244, 193, and 208 are detected in the full, soft, and hard bands, respectively. The Chandra observation covers a total area of 335 arcmin2 and reaches flux limits over the central few square arcmins of ∼3 × 10−16, 6 × 10−17, and 2 × 10−16 erg cm−2 s−1 in the full, soft, and hard bands, respectively This makes J1030 field the fifth deepest extragalactic X-ray survey to date. The field is part of the Multiwavelength Survey by Yale-Chile (MUSYC), and is also covered by optical imaging data from the Large Binocular Camera (LBC) at the Large Binocular Telescope (LBT), near-infrared imaging data from the Canada France Hawaii Telescope WIRCam (CFHT/WIRCam), and Spitzer IRAC. Thanks to its dense multi-wavelength coverage, J1030 represents a legacy field for the study of large-scale structures around distant accreting supermassive black holes. Using a likelihood ratio analysis, we associate multi-band (r, z, J, and 4.5 μm) counterparts for 252 (98.4%) of the 256 Chandra sources, with an estimated reliability of 95%. Finally, we compute the cumulative number of sources in each X-ray band, finding that they are in general agreement with the results from the Chandra Deep Fields.

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PELICAN: deeP architecturE for the LIght Curve ANalysis

Astronomy and Astrophysics ◽

10.1051/0004-6361/201834473 ◽

2019 ◽

Vol 627 ◽

pp. A21 ◽

Cited By ~ 9

Author(s):

Johanna Pasquet ◽

Jérôme Pasquet ◽

Marc Chaumont ◽

Dominique Fouchez

Keyword(s):

Light Curve ◽

Sampling Rate ◽

Real Data ◽

Curve Analysis ◽

Irregular Sampling ◽

Light Curves ◽

Light Curve Analysis ◽

Deep Architecture ◽

Deep Fields

We developed a deeP architecturE for the LIght Curve ANalysis (PELICAN) for the characterization and the classification of supernovae light curves. It takes light curves as input, without any additional features. PELICAN can deal with the sparsity and the irregular sampling of light curves. It is designed to remove the problem of non-representativeness between the training and test databases coming from the limitations of the spectroscopic follow-up. We applied our methodology on different supernovae light curve databases. First, we tested PELICAN on the Supernova Photometric Classification Challenge for which we obtained the best performance ever achieved with a non-representative training database, by reaching an accuracy of 0.811. Then we tested PELICAN on simulated light curves of the LSST Deep Fields for which PELICAN is able to detect 87.4% of supernovae Ia with a precision higher than 98%, by considering a non-representative training database of 2k light curves. PELICAN can be trained on light curves of LSST Deep Fields to classify light curves of the LSST main survey, which have a lower sampling rate and are more noisy. In this scenario, it reaches an accuracy of 96.5% with a training database of 2k light curves of the Deep Fields. This constitutes a pivotal result as type Ia supernovae candidates from the main survey might then be used to increase the statistics without additional spectroscopic follow-up. Finally we tested PELICAN on real data from the Sloan Digital Sky Survey. PELICAN reaches an accuracy of 86.8% with a training database composed of simulated data and a fraction of 10% of real data. The ability of PELICAN to deal with the different causes of non-representativeness between the training and test databases, and its robustness against survey properties and observational conditions, put it in the forefront of light curve classification tools for the LSST era.

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The Canada-France deep fields survey–II: Lyman-break galaxies and galaxy clustering atz $\mathsf{\sim3}$

Astronomy and Astrophysics ◽

10.1051/0004-6361:20031181 ◽

2003 ◽

Vol 409 (3) ◽

pp. 835-850 ◽

Cited By ~ 54

Author(s):

S. Foucaud ◽

H. J. McCracken ◽

O. Le Fèvre ◽

S. Arnouts ◽

M. Brodwin ◽

...

Keyword(s):

Galaxy Clustering ◽

Lyman Break Galaxies ◽

Deep Fields

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Obscured AGN

Proceedings of the International Astronomical Union ◽

10.1017/s1743921314003275 ◽

2013 ◽

Vol 9 (S304) ◽

pp. 43-43

Author(s):

Amy Barger

Keyword(s):

Growth Rate ◽

Black Hole ◽

Substantial Fraction ◽

X Ray ◽

James Clerk Maxwell ◽

Supermassive Black Hole ◽

Black Hole Growth ◽

Deep Fields ◽

Hole Growth

AbstractObscured AGN may correspond to a substantial fraction of the supermassive black hole growth rate. I will present new surveys with the SCUBA-2 instrument on the James Clerk Maxwell Telescope of the Chandra Deep Fields and discuss whether we can distinguish obscured AGN in hard X-ray and radio selected samples using submillimeter observations.

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