J/A+A/691/A138 S-PLUS Ultra-Short Survey DR1 (Perottoni+, 2024)
The S-PLUS Ultra-Short Survey: First data release.
Perottoni H.D., Placco V.M., Almeida-Fernandes F., Herpich F.R., Rossi S.,
Beers T.C., Smiljanic R., Amarante J.A.S., Limberg G., Werle A.,
Rocha-Pinto H.J., Beraldo e Silva L., Daflon S., Alvarez-Candal A.,
Oliveira Schwarz G.B., Schoenell W., Ribeiro T., Kanaan A.
<Astron. Astrophys. 691, A138 (2024)>
=2024A&A...691A.138P 2024A&A...691A.138P (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Stars, bright ; Stars, metal-deficient ;
Photometry, narrow-band
Keywords: techniques: photometric - techniques: spectroscopic - catalogs -
surveys - stars: Population II
Abstract:
This paper presents the first public data release of the S-PLUS
Ultra-Short Survey (USS), a photometric survey with short exposure
times, cove ring approximately 9300deg2 of the Southern sky. The USS
utilizes the Javalambr e 12-band magnitude system, including narrow
and medium-band and broad-band filt ers targeting prominent stellar
spectral features. The primary objective of the USS is to identify
bright, extremely metal-poor (EMP; [Fe/H]≤-3) and ultra-metal-poor
(UMP; [Fe/H]≤-4) stars for further analysis using medium- and
high-resolution spectroscopy.
This paper provides an overview of the survey observations,
calibration method, data quality, and data products. Additionally, it
presents the selection of EMP and UMP candidates.
The data from the USS were reduced and calibrated using the same
methods as presented in the S-PLUS DR2. An additional step was
introduced, accounting for the offset between the observed magnitudes
off the USS and the predicted magnitudes from the very low-resolution
Gaia XP spectra.
This first release contains data for 163 observed fields totaling
∼324deg2 along the Celestial Equator. The magnitudes obtained from
the USS are well-calibrated, showing a difference of ∼15mmag compared
to the predicted magnitudes by the GaiaXPy toolkit. By combining
colors and magnitudes, 140 candidates for EMP or UMP have been
identified for follow-up studies.
The S-PLUS USS DR1 is an important milestone in the search for bright
metal-poor stars, with magnitudes in the range 10<r≤14. The USS is an
ongoing survey; in the near future, it will provide many more bright
metal-poor candidate stars for spectroscopic follow-up.
Description:
The S-PLUS project, facilitated by the S-PLUS Consortium, was built to
be the Southern Hemisphere counterpart of J-PLUS, and is operated in
collaboration with the Astronomy Department at the University of Sao
Paulo, Brazil. The S-PLUS survey includes various sub-surveys, one of
which is known as the S-PLUS Ultra-Short Survey (USS). The USS is an
imaging survey that covers the same area as the overall S-PLUS Main
Survey, but with much shorter exposure times. As in the S-PLUS Main
survey, USS employs a set of 12 bands (seven narrow and medium-band
filters and five broad-band filters) for its observations, enabling
comprehensive characterization of objects by imaging them in different
regions of the optical spectra, with the narrow and medium-band
filters placed on crucial elemental absorption lines.
Catalog of USS DR1 EMP (extremely metal-poor) and UMP (ultra
metal-poor) candidates.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tableb1.dat 286 140 Catalog of USS DR1 EMP and UMP candidates
--------------------------------------------------------------------------------
See also:
https://splus.cloud : S-PLUS Home Page
Byte-by-byte Description of file: tableb1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 33 A33 --- ID Identification
(SDR1SHORTS-STRIPE82NNNN_NNNNNNN)
35- 45 F11.7 deg RAdeg Right ascension (J2000)
47- 58 F12.9 deg DEdeg Declination (J2000)
60- 77 F18.15 mag umag u band (3533Å) magnitude (AB) corrected
for interstellar medium extinction
79- 96 F18.15 mag J0378mag J0378 (3773Å) band magnitude (AB) corrected
for interstellar medium extinction
98-115 F18.15 mag J0395mag J0395 (3940Å) band magnitude (AB) corrected
for interstellar medium extinction
117-134 F18.15 mag J0410mag J0410 (4095Å) band magnitude (AB) corrected
for interstellar medium extinction
136-153 F18.15 mag J0430mag J0430 (4292Å) band magnitude (AB) corrected
for interstellar medium extinction
155-172 F18.15 mag gmag g (4758Å) band magnitude (AB) corrected
for interstellar medium extinction
174-191 F18.15 mag J0515mag J0515 (5133Å) band magnitude (AB) corrected
for interstellar medium extinction
193-210 F18.15 mag rmag r (6251Å) band magnitude (AB) corrected
for interstellar medium extinction
212-229 F18.15 mag J0660mag J0660 (6613Å) band magnitude (AB) corrected
for interstellar medium extinction
231-248 F18.15 mag imag i (7670Å)band magnitude (AB) corrected
for interstellar medium extinction
250-267 F18.15 --- J0861mag J0861 (8607Å) band magnitude (AB) corrected
for interstellar medium extinction
269-286 F18.15 --- zmag z (8936Å) band magnitude (AB) corrected
for interstellar medium extinction
--------------------------------------------------------------------------------
Acknowledgements:
Helio Perottoni, hperottoni(at)gmail.com
(End) Patricia Vannier [CDS] 17-Sep-2024