J/AJ/166/102 SFACT. III. SFF01 -10 and -15 spectral data (Carr+, 2023)
The Star Formation Across Cosmic Time (SFACT) Survey.
III. Spectroscopy of the Initial Catalog of Emission-line Objects.
Carr D.J., Sieben J., Salzer J.J., Brunker S.W., Cousins B.
<Astron. J., 166, 102 (2023)>
=2023AJ....166..102C 2023AJ....166..102C
ADC_Keywords: Galaxies, dwarf; Star Forming Region; Spectra, optical;
Redshifts
Keywords: Galaxy abundances ; Blue compact dwarf galaxies ; Dwarf
irregular galaxies ; Emission-line galaxies ; Galaxy evolution ;
Galaxy spectroscopy ; LINER galaxies ; Seyfert galaxies ;
Quasars ; Starburst galaxies ; Surveys ; Star formation
Abstract:
The Star Formation Across Cosmic Time (SFACT) survey is a new
narrowband survey designed to detect emission-line galaxies (ELGs) and
quasi-stellar objects (QSOs) over a wide range of redshifts in
discrete redshift windows. The survey utilizes the WIYN 3.5m telescope
and the Hydra multifiber positioner to perform efficient follow-up
spectroscopy on galaxies identified in the imaging part of the survey.
Because the objects in the SFACT survey are selected by their strong
emission lines, it is possible to obtain useful spectra for even the
faintest of our sources (r∼25). Here, we present the 453 objects that
have spectroscopic data from the three SFACT pilot-study fields, 415
of which are confirmed ELGs. The methodology for processing and
measuring these data is outlined in this paper, and example spectra
are displayed for each of the three primary emission lines used to
detect objects in the survey (Hα, [OIII]λ5007, and
[OII]λ3727). Spectra of additional QSOs and
nonprimary-emission-line detections are also shown as examples. The
redshift distribution of the pilot-study sample is examined, and the
ELGs are placed in different emission-line diagnostic diagrams in
order to distinguish the star-forming galaxies from the active
galactic nuclei.
Description:
All spectroscopic data obtained for SFACT were acquired using the WIYN
3.5m telescope located at Kitt Peak National Observatory. This section
will cover the instrumentation and observational procedures associated
with the spectroscopic part of the survey. The spectroscopic data for
the SFACT pilot-study fields were obtained during observing runs in
2017 November, 2018 October, 2019 August, 2019 October, and 2021
October. With our chosen spectroscopic setup, the observed wavelength
range for our follow-up spectra is roughly 4760-7580Å.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 124 132 SFF01 Spectral Data Table
table2.dat 124 216 SFF10 Spectral Data Table
table3.dat 124 185 SFF15 Spectral Data Table
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See also:
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
J/ApJS/95/387 : Universidad Complutense de Madrid list 1 (Zamorano+ 1994)
J/ApJS/105/343 : Universidad Complutense de Madrid list 2 (Zamorano+ 1996)
J/A+AS/135/511 : The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)
J/A+AS/142/417 : Hamburg/SAO Survey for ELGs. III. (Hopp+, 2000)
J/AJ/121/66 : KISS Hα survey list 1 (Salzer+, 2001)
J/AJ/123/1292 : KISS III. [O III]-selected survey list (Salzer+, 2002)
J/ApJ/668/853 : Spectro UltraStrong Emission Line galaxies (Kakazu+, 2007)
J/AJ/139/279 : Outlying HII regions in HI-selected galaxies (Werk+, 2010)
J/AJ/143/145 : Emission-line objects ALFALFA Halpha survey (Kellar+, 2012)
J/MNRAS/428/1128 : UDS/COSMOS HiZELS galaxies (Sobral+, 2013)
J/ApJ/880/7 : Census of Local Universe survey. I. CLU-Halpha (Cook+, 2019)
J/AJ/160/242 : The Hα dots survey. II. 119 new dots (Salzer+, 2020)
Byte-by-byte Description of file: table[123].dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- ObjID Unique SFACT object identifier (1)
18- 42 A25 --- SFACT SFACT IAU approved coordinate-based
designation
44- 52 F9.5 deg RAdeg Right Ascension, decimal degrees (ICRS) (2)
54- 61 F8.5 deg DEdeg Declination, decimal degrees (ICRS) (2)
63- 66 A4 --- Type Activity Type (3)
68- 74 F7.5 --- zspec ? Spectroscopic redshift (4)
76- 79 I4 0.1nm Line ? Emission Line, Angstroms (5)
81- 81 A1 --- f_logNIIHa Flag on logNIIHa (6)
83- 88 F6.3 [-] logNIIHa ? log, [NII]/Hα line ratio
90- 94 F5.3 [-] e_logNIIHa ? Uncertainty in logNIIHa
96- 96 A1 --- f_logOIIIHb Flag on logOIIIHb (6)
98-103 F6.3 [-] logOIIIHb ? log, [OIII]/Hβ line ratio
105-109 F5.3 [-] e_logOIIIHb ? Uncertainty in logOIIIHb
111-111 A1 --- f_logOIIHb Flag on logOIIHb (6)
113-118 F6.3 [-] logOIIHb ? log, [OII]/Hβ line ratio
120-124 F5.3 [-] e_logOIIHb ? Uncertainty in logOIIHb
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Note (1): This is a unique ID for each object and contains three parts.
The first part represents the field where the object is located
(e.g., SFF01), while the second designates the filter within which
the source was detected. The third contains information on which
quadrant of the field the object is located in (A, B, C, or D)
followed by a number that represents the order in which the image
processing software finds the object in the field.
Note (2): The SFACT coordinates are derived from an astrometric solution
applied to the survey imaging data based on the Gaia database, which
is on the ICRS. The RMS scatter for individual stars is ?0.15-0.20 arcsec.
Note (3): Activity type of each source detected by the survey,
derived by visual inspection of the spectra, supplemented by use
of line diagnostic diagrams --
ELG = emission-line galaxies;
FD = false detection -- no obvious emission lines in their spectra;
HII = H II regions in nearby disk galaxies;
LIN = low-ionization nuclear emission region, LINER;
QSO = quasar;
SFG = star-forming galaxy (inc, Starburst Nucleus galaxies,
blue compact dwarfs, Green Pea galaxies, etc);
Star = Star;
Sy2 = Seyfert 2.
Note (4): The characteristic uncertainties in our redshift
measurements are 0.00003 to 0.00005, based on the RMS scatter of
the redshifts measured from individual lines in a given spectrum
(see Section 4.2).
Note (5): That emission line (in Angstroms) responsible for the
detection of each SFACT object --
1549 = CIV;
1908 = CIII];
2798 = MgII;
3727 = [OII];
3869 = [NIII];
4861 = Hβ;
4959 = [OIII];
5007 = [OIII];
6563 = Hα.
Note (6): For line ratios where one or both lines are Category 2
re-examination measurements (described in Section 4.2), the
uncertainies in the line ratios will be larger; these are
marked with the flag of "u".
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History:
From electronic version of the journal
References:
Salzer et al. Paper I : 2023AJ....166...81S 2023AJ....166...81S
Sieben et al. Paper II : 2023AJ....166..101S 2023AJ....166..101S Cat. J/AJ/166/101
(End) Prepared by [AAS], Coralie Fix [CDS], 22-Mar-2024