J/AJ/155/189 LAMOST Quasar Survey: quasar properties from DR2&3 (Dong+, 2018)
The Large Sky Area Multi-Object Fibre Spectroscopic Telescope (LAMOST) Quasar
Survey: quasar properties from data release two and three.
Dong X.Y., Wu X.-B., Ai Y.L., Yang J.Y., Yang Q., Wang F., Zhang Y.X.,
Luo A.L., Xu H., Yuan H.L., Zhang J.N., Wang M.X., Wang L.L., Li Y.B.,
Zuo F., Hou W., Guo Y.X., Kong X., Chen X.Y., Wu Y., Yang H.F., Yang M.
<Astron. J., 155, 189-189 (2018)>
=2018AJ....155..189D 2018AJ....155..189D (SIMBAD/NED BibCode)
ADC_Keywords: QSOs ; Spectroscopy ; Redshifts ; Equivalent widths ; Surveys
Keywords: catalogs - quasars: emission lines - quasars: general - surveys
Abstract:
This is the second installment for the Large Sky Area Multi-Object
Fibre Spectroscopic Telescope (LAMOST) Quasar Survey, which includes
quasars observed from 2013 September to 2015 June. There are 9024
confirmed quasars in DR2 and 10911 in DR3. After cross-match with the
Sloan Digital Sky Survey (SDSS) quasar catalogs and NED, 12126 quasars
are discovered independently. Among them, 2225 quasars were released
by SDSS DR12 QSO catalog in 2014 after we finalized the survey candidates.
1801 sources were identified by SDSS DR14 as QSOs. The remaining 8100
quasars are considered as newly founded, and among them, 6887 quasars
can be given reliable emission line measurements and the estimated
black hole masses. Quasars found in LAMOST are mostly located at
low-to-moderate redshifts, with a mean value of 1.5. The highest redshift
observed in DR2 and DR3 is 5. We applied emission line measurements to
Hα, Hβ, Mg II, and C IV. We deduced the monochromatic
continuum luminosities using photometry data, and estimated the virial
black hole masses for the newly discovered quasars. Results are
compiled into a quasar catalog, which will be available online.
Description:
The Large Sky Area Multi-Object Fibre Spectroscopic Telescope (LAMOST)
Quasar Survey is conducted under the LAMOST ExtraGAlactic Survey (LEGAS;
Zhao et al. 2012RAA....12..723Z 2012RAA....12..723Z). Its quasar candidates are selected based
on multi-color photometry and data-mining. The regular survey began in
2012 September and will continue for the next five to six years. This paper
is the second installment in the series of LAMOST quasar survey, after
the pilot observations (Wu et al. 2010RAA....10..737W 2010RAA....10..737W, 2010RAA....10..745W 2010RAA....10..745W)
and data release one (Ai et al. 2016, J/AJ/151/24, Paper I). Here, we
report LAMOST quasar survey data releases two and three, which include
quasars observed between 2013 September and 2015 June.
The LAMOST, also known as Guoshoujing Telescope, is a 4 m reflecting
Schmidt telescope located at Xinglong Observatory, China (Cui et al.
2012RAA....12.1197C 2012RAA....12.1197C; Zhao et al. 2012RAA....12..723Z 2012RAA....12..723Z). It is equipped with
4000 fibers across a 5° field of view. LAMOST has two sets of
spectrographs. The blue channel covers the spectrum from 3700 to 5900Å,
while the red channel covers the spectrum from 5700 to 9000Å. The
spectral resolution R is about 1800 over the entire wavelength range.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table12.dat 732 9024 The LAMOST Quasar Survey Data Release Two Quasar
Catalog
table13.dat 732 10911 The LAMOST Quasar Survey Data Release Three
Quasar Catalog
--------------------------------------------------------------------------------
See also:
VII/260 : The SDSS-DR7 quasar catalog (Schneider+, 2010)
V/139 : The SDSS Photometric Catalog, Release 9 (Adelman-McCarthy+, 2012)
VII/270 : SDSS quasar catalog: tenth data release (Paris+, 2014)
V/146 : LAMOST DR1 catalogs (Luo+, 2015)
V/149 : LAMOST DR2 catalogs (Luo+, 2016)
VII/279 : SDSS quasar catalog: twelfth data release (Paris+, 2017)
V/153 : LAMOST DR4 catalogs (Luo+, 2018)
J/AJ/131/2766 : Quasar luminosity function from SDSS-DR3
(Richards+, 2006)
J/AJ/145/159 : LAMOST. II. ugriz photometry of 526 new quasars
(Huo+, 2013)
J/other/RAA/15.1438 : LAMOST new QSOs in M31 and M33 vicinity (Huo+, 2015)
J/AJ/151/24 : LAMOST quasar survey: quasar properties from the DR1
(Ai+, 2016)
Byte-by-byte Description of file: table12.dat table13.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 I9 --- ObsID [102141/347512058] Observation identifier
in LAMOST database (OBSID)
11- 29 A19 --- Target Target designation in LAMOST database
(JHHMMSS.ss+DDMMSS.s, J2000)
(DESIGNATION)
31- 40 F10.6 deg RAdeg Right Ascension in decimal degrees
(J2000) (RA)
42- 50 F9.6 deg DEdeg Declination in decimal degrees (J2000)
(DEC)
52- 69 A18 --- PlanId Spectroscopic plan identification
(PLANID)
71- 72 I2 --- spId [1/16]? Spectrograph identification
(SPID)
74- 76 I3 --- FiberId [0/250] Fiber number of the spectrum
(FIBERID)
78- 82 I5 d MJD [55858/57165] Modified Julian Date of
the spectroscopic observation (MJD)
84- 85 I2 --- Source Source of quasar candidate (SOURCE_FLAG)
(1)
90- 97 F8.4 mag iMag [-35.3985/-1.8353]? Absolute i-band
magnitude with K-correction to z=2
following Richards et al.
(2006, J/AJ/131/2766) (Mi)
99-104 A6 --- Class Classification given by visual inspection
(CLASS_VI)
106 I1 --- f_Class [0/1] Classification flag (1=Uncertain
classification) (CLASS_FLAG)
108-114 F7.4 --- z-pipeline [-0.0041/4.088]?=-9.9999 Redshift given
by LAMOST pipeline (Z_PIPELINE)
116-122 F7.4 --- z-vi [0/5.0087]?=99.9999 Redshift given by
visual inspection (Z_VI)
124 I1 --- QF-z [1/9]?=0 Redshift quality flag (Z_FLAG)
(2)
126-133 F8.4 --- S/N-Spec [-1.0463/134.872] Median signal-to-noise
ratio per pixel of the spectrum
(SNR_SPEC)
135-145 E11.6 km/s FWHM-Hab [0/14230]? Full width at half maximum
of broad Hα (FWHMBROADHA)
147-157 E11.6 0.1nm EW-Hab [0/1.63e+11]? Rest-frame equivalent
width of broad Hα (Å)
(EWBROADHA)
159-169 E11.6 km/s FWHM-Han [0/1200]? Full width at half maximum of
narrow Hα (FWHMNARROWHA)
171-181 E11.6 0.1nm EW-Han [0/3.94e+10]? Rest-frame equivalent width
of narrow Hα (Å) (EWNARROWHA)
183-193 E11.6 0.1nm EW-NII6584 [0/1.84e+10]? Rest-frame equivalent width
of [N II]6584 (Å) (EWNII6585)
195-205 E11.6 0.1nm EW-SII6718 [0/5290.64]? Rest-frame equivalent width
of [S II]6718 (Å) (EWSII6718)
207-217 E11.6 0.1nm EW-SII6732 [0/1.12e+07]? Rest-frame equivalent width
of [S II]6732 (Å) (EWSII6732)
219-229 E11.6 0.1nm EW-FeHa [0/32039.6]? Rest-frame equivalent width
of Fe within 6000-6500Å (Å)
(EWFEHA)
231-233 I3 --- NPix-Ha [0/252] Number of good pixels at the
rest-frame 6400-6765Å (LINENPIXHA)
235-243 F9.5 --- S/N-Ha [0/273.564]? Median signal-to-noise ratio
per pixel at the rest-frame
6400-6765Å (LINEMEDSN_HA)
245-252 F8.5 --- chi2-Ha [-1/32.6007] Reduced χ2 of Hα
emission line fit (LINEREDCHI2HA)
254-255 I2 --- QF-Ha [-1/1]? Quality flag of Hα fitting
(LINEFLAGHA) (3)
257-267 E11.6 km/s FWHM-Hb [0/18927.2]? Full width at half maximum
of broad Hβ (FWHMBROADHB)
269-279 E11.6 0.1nm EW-Hb [0/4.95e+17]? Rest-frame equivalent width
of broad Hβ (Å) (EWBROADHB)
281-291 E11.6 km/s FWHM-Hbn [0/1200]? Full width at half maximum of
narrow Hβ (FWHMNARROWHB)
293-303 E11.6 0.1nm EW-Hbn [0/7.09e+15]? Rest-frame equivalent width
of narrow Hβ (Å) (EWNARROWHB)
305-315 E11.6 0.1nm EW-OIII4959 [0/1.64e+17]? Rest-frame equivalent width
of [O III]4959 (Å) (EWOIII4959)
317-327 E11.6 0.1nm EW-OIII5007 [0/5.06e+17]? Rest-frame equivalent width
of [O III]5007 (Å) (EWOIII5007)
329-339 E11.6 0.1nm EW-FeHb [0/5.63e+18]? Rest-frame equivalent width
of Fe within 4435-4685Å (Å)
(EWFEHB)
341-343 I3 --- NPix-Hb [0/346] Number of good pixels at the
rest-frame 4750-4950Å (LINENPIXHB)
345-347 I3 --- S/N-Hb [0/136]? Median signal-to-noise ratio per
pixel at the rest-frame 4750-4950Å
(LINEMEDSN_HB)
349-356 F8.5 --- chi2-Hb [-1/71.4036]? Reduced χ2 of Hβ
emission line fit (LINEREDCHI2HB)
358-359 I2 --- QF-Hb [-1/1]? Quality flag of Hβ fitting
(LINEFLAGHB) (3)
361-371 E11.6 km/s FWHM-MGII2796b [0/270093]? Full width at half maximum of
the broad Mg II 2796
(FWHMBROADMGII_2796)
373-383 E11.6 0.1nm EW-MGII2796b [0/3.47e+13]? Rest-frame equivalent
width of the broad Mg II 2796 (Å)
(EWBROADMGII_2796)
385-395 E11.6 km/s FWHM-MGII2796n [0/900]? Full width at half maximum of
the narrow Mg II 2796
(FWHMNARROWMGII_2796)
397-407 E11.6 0.1nm EW-MGII2796n [0/9.86e+09]? Rest-frame equivalent
width of the narrow Mg II 2796 (Å)
(EWNARROWMGII_2796)
409-419 E11.6 km/s FWHM-MGIIb [0/270093]? Full width at half maximum of
the whole broad Mg II (FWHMBROADMGII)
421-431 E11.6 0.1nm EW-MGIIb [0/5.82e+13]? Rest-frame equivalent
width of the whole broad Mg II (Å)
(EWBROADMGII)
433-443 E11.6 km/s FWHM-MGII [0/269264]? Full width at half maximum of
the whole Mg II emission line
(FWHM_MGII)
445-455 E11.6 0.1nm EW-MGII [0/5.82e+13]? Rest-frame equivalent
width of the whole Mg II (EW_MGII)
457-467 E11.6 0.1nm EW-FeMGII [0/1.24145e+06]? Rest-frame equivalent
width of Fe within 2200-3090Å (Å)
(EWFEMGII)
469-471 I3 --- NPix-MGII [0/310] Number of good pixels at the
rest-frame 2700-2900Å
(LINENPIXMGII)
473-482 F10.5 --- S/N-MGII [0/1813.21]? Median signal-to-noise ratio
per pixel at the rest-frame
2700-2900Å (LINEMEDSN_MGII)
484-492 F9.5 --- chi2-MGII [-1/274.761]? Reduced χ2 of Mg II
emission line fit (LINEREDCHI2MGII)
494-495 I2 --- QF-MGII [-1/1]? Quality flag of Mg II fitting
(LINEFLAGMGII) (3)
497-507 E11.5 km/s FWHM-CIVb [0/11605]? Full width at half maximum of
the broad C IV (FWHMBROADCIV)
509-519 E11.5 0.1nm EW-CIVb [0/6.85e+19]? Rest-frame equivalent width
of the broad C IV (Å) (EWBROADCIV)
521-531 E11.5 km/s FWHM-CIVn [0/1200]? Full width at half maximum of
the narrow C IV (FWHMNARROWCIV)
533 I1 0.1nm EW-CIVn [0]? Rest-frame equivalent width of the
narrow C IV (Å) (EWNARROWCIV)
535-545 E11.5 km/s FWHM-CIV [0/11605]? Full width at half maximum of
the whole C IV (FWHM_CIV)
547-558 E12.6 0.1nm EW-CIV [-4.72e+25/2.46e+31]? Rest-frame
equivalent width of the whole C IV
(Å) (EW_CIV)
560-562 I3 --- NPix-CIV [0/281] Number of good pixels at the
rest-frame 1500-1600Å (LINENPIXCIV)
564-571 F8.5 --- S/N-CIV [0/65.9714]? Median signal-to-noise ratio
per pixel at the rest-frame
1500-1600Å (LINEMEDSN_CIV)
573-582 F10.5 --- chi2-CIV [-1/2089.66]? Reduced χ2 of C IV
emission line fit (LINEREDCHI2CIV)
584-585 I2 --- QF-CIV [-1/1]? Quality flag of C IV fitting
(LINEFLAGCIV) (3)
587-594 F8.5 --- alphal1 [-5.50547/0]? Wavelength power-law index
from 1300 to 4661Å αlambda
(ALPHA1)
596-603 F8.5 --- alphal2 [-4.1927/0]? Wavelength power-law index
from 4661Å toward the red end of the
spectrum αlambda (ALPHA2)
605-615 E11.5 --- chi2-Cont [0/865420]? Reduced χ2 of continuum
fitting (CONT_CHI2)
617 I1 --- QF-Cont [0/1]? Quality flag of continuum fitting
(CONT_FLAG) (4)
619-626 F8.5 10-7W logL1350 [0/49.33483]? Monochromatic luminosity at
1350Å (in erg/s) (LOGL1350)
628-635 F8.5 10-7W e_logL1350 [0/11.3802]? Error of logL1350 (in erg/s)
(LOGL1350_ERR) (5)
637-644 F8.5 10-7W logL3000 [-6.46228/48.4736]? Monochromatic
luminosity at 3000Å (in erg/s)
(LOGL3000)
646-653 F8.5 10-7W e_logL3000 [0/12.1695]? Error of logL3000 (in erg/s)
(LOGL3000_ERR) (5)
655-662 F8.5 10-7W logL5100 [0/48.4763]? Monochromatic luminosity at
5100Å (in erg/s) (LOGL5100)
664-671 F8.5 10-7W e_logL5100 [0/12.8869]? Error of logL5100 (in erg/s)
(LOGL5100_ERR) (5)
673-680 F8.5 Msun logMBH-Hb [0/10.0117]? Virial BH mass based on
Hβ (LOGMBH_HB)
682-688 F7.5 Msun e_logMBH-Hb [0/0.06382]? Error of logMBH-Hb
(LOGMBHERRHB) (5)
690-691 I2 --- q_logMBH-Hb [-1/1]? Reliability of logMBH-Hb
(LOGMBHHBFLAG) (6)
693-700 F8.5 Msun logMBH-MGII [0/12.6728]? Virial BH mass based on
Mg II (LOGMBH_MGII)
702-709 F8.5 Msun e_logMBH-MGII [-1/0.13668]? Error of logMBH-MGII
(LOGMBHERRMGII) (5)
711-712 I2 --- q_logMBH-MGII [-1/1]? Reliability of logMBH-MGII
(LOGMBHMGIIFLAG) (6)
714-721 F8.5 Msun logMBH-CIV [-1/11.1091]? Virial BH mass based on
C IV (LOGMBH_CIV)
723-729 F7.5 Msun e_logMBH-CIV [0/0.19674]? Error of logMBH-CIV
(LOGMBHERRCIV) (5)
731-732 I2 --- q_logMBH-CIV [-1/1]? Reliability of logMBH-CIV
(LOGMBHCIVFLAG) (6)
--------------------------------------------------------------------------------
Note (1): SOURCE_FLAG is a 7-bit binary digit. The first three bits indicate
whether the quasar is already reported by SDSS or NED (i.e., "011" in
SDSS DR7, DR9 or DR10, "001" in DR12, "100" reported in DR14, "010" reported
in NED but not in SDSS, and "000" neither reported by SDSS nor NED). The two
bits in the middle indicate how the quasar candidate is selected (i.e., "00"
infrared-optical color selected, "01" data-mining selected, "10" object not
included in LAMOST LEGAS quasar survey sample but identified as quasar). The
last two bits indicate whether the quasar is overlapped with M31/M33 field
("00" not overlapped, "01" object already reported in Huo et al. (2015,
J/other/RAA/15.1438), "10" object in M31/M33 field but not in Huo et al. 2015,
J/other/RAA/15.1438). For example SOURCE_FLAG=64. "64" written in binary
system is "1000000". It means the quasar has already been reported by DR14,
it was selected via infrared-optical color selection, and is not within
M31/M33 field.
Note (2): Redshift quality flag as follows:
1 = If the value of redshift is uncertain (e.g., only one emission line
available);
9 = If the spectrum is likely a quasar but too noisy to yield a redshift.
Note (3): As mentioned in Section 4.5, the MPFIT package (Markwardt
2009ASPC..411..251M 2009ASPC..411..251M) is used to perform χ2-minimization using the
Levenberg-Marquardt technique.
Quality flag as follows:
0 = When the fitting converges;
-1 = Fitting without converged results. The un-converged fits are usually
caused by low S/N, too few good pixels in the fitting region, or peculiar
continuum and emission line properties. If Hα/Hβ/Mg II/C IV is
outside the observational frame, quality flag=-1;
1 = After fitting, we visually inspect each fitting result with quality
flag=0. For those with clearly over-subtracted continuum, we changed
their flag from 0 to 1 to flag an unreliable fit. Values of QF-CIV are
also changed to 1 for those BAL candidates.
Note (4): As mentioned in Section 5, Python PYTOOLS.NMPFIT is used to perform
χ2-minimization with the Levenberg-Marquardt algorithm.
Quality flag as follows:
0 = When the fitting converges;
1 = If the fitting cannot converge. The un-converged fitting usually happens
when the SDSS 5-band magnitudes form a peculiar shape and, therefore,
cannot be fitted with the composite spectrum.
Note (5): The monochromatic luminosity and BH mass errors are calculated using
Monte-Carlo simulation.
Note (6): As BH mass is estimated using FWHM and monochromatic continuum
luminosity, the flags of the BH mass are the combinations of the emission line
fitting flags and the continuum fitting flags as shown below. When the
f_logMBH=-1, there is no available BH mass estimate. If the f_logMBH=1, the
BH mass estimate should be used with caution.
The determination of BH mass flags (Table 2 from this paper):
------------------------------
QF-Cont | LINE_FLAG | q_logMBH
------------------------------
0 | 0 | 0
0 | 1 | 1
0 | -1 | -1
1 | 0 | 1
1 | -1 | -1
1 | 1 | 1
------------------------------
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History:
From electronic version of the journal
References:
Ai et al. DR1 Paper I. 2016AJ....151...24A 2016AJ....151...24A Cat. J/AJ/151/24
Dong et al. DR2+3 Paper II. 2018AJ....155..189D 2018AJ....155..189D This catalog
Yao et al. DR4+5 Paper III. 2019ApJS..240....6Y 2019ApJS..240....6Y Cat. J/ApJS/240/6
Jin et al. DR6-9 Paper IV. 2023ApJS..265...25J 2023ApJS..265...25J Cat. J/ApJS/265/25
(End) Tiphaine Pouvreau [CDS] 30-Nov-2018