J/ApJ/930/39 128 new Herbig stars (Vioque+, 2022)
Identification and spectroscopic characterization of 128 new Herbig stars.
Vioque M., Oudmaijer R.D., Wichittanakom C., Mendigutia I., Baines D.,
Panic O., Iglesias D., Miley J., Perez-Martinez R.
<Astrophys. J. 930, 39 (2022)>
=2022ApJ...930...39V 2022ApJ...930...39V (SIMBAD/NED BibCode)
ADC_Keywords: Stars, pre-main sequence ; Stars, emission ;
Effective temperatures ; Stars, distances ; Stars, masses ;
Stars, ages ; Equivalent widths ; Spectra, optical
Keywords: Herbig Ae/Be stars - star formation - pre-main sequence stars -
young stellar objects - massive stars - stellar accretion -
hertzsprung Russell diagram - emission line stars
Abstract:
We present optical spectroscopy observations of 145 high-mass
pre-main-sequence candidates from the catalog of Vioque et al. (2020,
PhD thesis University of Leeds) From these, we provide evidence for
the Herbig nature of 128 sources. This increases the number of known
objects of the class by ∼50%. We determine the stellar parameters of
these sources using the spectra and Gaia EDR3 data. The new sources
are well distributed in mass and age, with 23 sources between 4 and
8M☉ and 32 sources above 8M☉. Accretion rates are inferred
from Hα and Hβ luminosities for 104 of the new Herbigs.
These accretion rates, combined with previous similar estimates, allow
us to analyze the accretion properties of Herbig stars using the
largest sample ever considered. We provide further support to the
existence of a break in accretion properties at ∼3-4M☉, which
was already reported for the previously known Herbig stars. We
re-estimate the potential break in accretion properties to be at
3.87-0.96+0.38M☉. As observed for the previously known
Herbig stars, the sample of new Herbig stars independently suggests
intense inner-disk photoevaporation for sources with masses above
∼7M☉. These observations provide robust observational support to
the accuracy of the Vioque et al. (2020, PhD thesis University of
Leeds) catalog of Herbig candidates.
Description:
A total of 145 Herbig candidates from the Vioque et al. (2020, PhD
thesis University of Leeds) catalog were observed in low- to
medium-resolution optical spectroscopy during three different
observing runs.
These 145 sources were selected because their absolute magnitudes
suggest that their stellar masses cover the Herbig mass regime in a
representative manner.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 137 145 Log of observations
tableb2.dat 173 145 Stellar parameters, distances and extinctions
for the 145 observed sources, ordered by name
tableb3.dat 109 145 Hα and Hβ observed equivalent widths
and line profiles
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name Identifier from this work, VOS NNNN
10- 28 I19 --- GaiaEDR3 Gaia EDR3 source identifier
30- 43 A14 --- AName Alternative name from literature
45- 46 I2 h RAh Right Ascension (ICRS) at Ep=2016.0 (1)
48- 49 I2 min RAm Right Ascension (ICRS) at Ep=2016.0 (1)
51- 55 F5.2 s RAs Right Ascension (ICRS) at Ep=2016.0 (1)
57 A1 --- DE- Declination sign (ICRS) at Ep=2016.0 (1)
58- 59 I2 deg DEd Declination (ICRS) at Ep=2016.0 (1)
61- 62 I2 arcmin DEm Declination (ICRS) at Ep=2016.0 (1)
64- 67 F4.1 arcsec DEs Declination (ICRS) at Ep=2016.0 (1)
69- 78 A10 "date" ObsBlue Observation date of Blue spectra (2)
79 A1 --- --- [;]
81- 82 I2 --- ObsBlue2 ? Second day of observation of Blue spectra
84- 93 A10 "date" ObsRed Observation date of Red spectra (2)
95- 98 I4 s ExpBlue1 Blue spectra first exposure time
99 A1 --- --- [;]
100-103 I4 s ExpBlue2 ? Blue spectra second exposure time
104 A1 --- --- [;]
105-107 I3 s ExpBlue3 ? Blue spectra third exposure time
109-112 I4 s ExpRed ? Red spectra exposure time
114-119 A6 --- Spec Spectrograph identifier
121-125 F5.2 mag Bpmag Gaia EDR3 Blue passband magnitude
127-131 F5.2 mag Gmag Gaia EDR3 white G passband magnitude
133-137 F5.2 mag Rpmag Gaia EDR3 Red passband magnitude
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Note (1): Coordinates from Gaia EDR3.
Note (2): YYYY-MM-DD format.
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Byte-by-byte Description of file: tableb2.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name Identifier from this work, VOS NNNN (1)
10 A1 --- f_SpType [b] Flag on SpType (2)
12- 20 A9 --- SpType Spectral type (3)
22 A1 --- f_Teff [b] Flag on Teff (2)
24- 28 I5 K Teff ? Effective temperature (3)
30- 34 I5 K E_Teff ? Upper uncertainty in Teff
36- 40 I5 K e_Teff ? Lower uncertainty in Teff
42- 48 F7.2 pc Dist Distance
50- 55 F6.2 pc E_Dist Upper uncertainty in Dist
57- 62 F6.2 pc e_Dist Lower uncertainty in Dist
64- 68 F5.3 mag AV ? V band extinction
70- 74 F5.3 mag E_AV ? Upper uncertainty in AV
76- 80 F5.3 mag e_AV ? Lower uncertainty in AV
82- 87 F6.3 [Lsun] logL* ? log stellar luminosity
89- 93 F5.3 [Lsun] E_logL* ? Upper uncertainty in logL*
95- 99 F5.3 [Lsun] e_logL* ? Lower uncertainty in logL*
101-106 F6.2 Rsun Rad ? Stellar radius
108-113 F6.2 Rsun E_Rad ? Upper uncertainty in Rad
115-120 F6.2 Rsun e_Rad ? Lower uncertainty in Rad
122-126 F5.2 Msun Mass ? Stellar mass
128-132 F5.2 Msun E_Mass ? Upper uncertainty in Mass
134-138 F5.2 Msun e_Mass ? Lower uncertainty in Mass
140-145 F6.3 Myr Age ? Stellar age
147-152 F6.3 Myr E_Age ? Upper uncertainty in Age
154-159 F6.3 Myr e_Age ? Lower uncertainty in Age
161-173 A13 --- Com Additional comments (G1)
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Note (1): VOS 1617 was observed with both IDS and EFOSC2 settings and was
assigned a B1.5 and a B3 spectral type respectively. Given the better
resolution of the IDS configuration and its smaller spectral type
uncertainty we consider the B1.5 spectral type determination for this object
in this work.
Note (2): Flag as follows:
b = Spectral type and/or Teff derived from spectra (Section 2.1)
Note (3): Approximated from the spectral derivations using the conversions
of Pecaut & Mamajek (2013ApJS..208....9P 2013ApJS..208....9P, Cat. J/ApJS/208/9) unless there
is a 'b' flag (see Note 2).
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Byte-by-byte Description of file: tableb3.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name Identifier from this work, VOS NNNN
10- 17 F8.2 0.1nm EWHa ? Observed Hα equivalent width
(in Angstroems unit)
19- 24 F6.2 0.1nm EWHb ? Observed Hβ equivalent width
(in Angstroems unit)
26- 33 F8.2 0.1nm EWcor ? Equivalent width correction
(in Angstroems unit) (1)
35- 37 A3 --- LP Line profile type (2)
39- 45 E7.2 Msun/yr dM/dt ? Accretion rate; see Sect. 5.
47- 53 E7.2 Msun/yr E_dM/dt ? Upper uncertainty in dM/dt
55- 61 E7.2 Msun/yr e_dM/dt ? Lower uncertainty in dM/dt
63 A1 --- l_IRExcess Limit flag on IRExcess
64- 72 E9.3 --- IRExcess ? IR excess; IR/stellar luminosity ratio
74- 82 E9.3 --- E_IRExcess ? Upper uncertainty in IRExcess
84- 92 E9.3 --- e_IRExcess ? Lower uncertainty in IRExcess
94- 95 A2 --- Flags Additional flags (3)
97-109 A13 --- Com Additional comments (G1)
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Note (1): The value which results from correcting the observed equivalent widths
from the typical line absorption equivalent width of each spectral type
(Sect. 5).
Note (2): Line profile type as follows:
s = single-peaked emission
d = double-peaked emission
rP = regular P-Cygni
iP = inverse P-Cygni
Note (3): Additional flags as follows:
b = The EWcor, LP, and Mdot values were derived from the Hβ line
and not the Hα line. HbEW values and Hb line profiles are
only presented when Hβ has emission and Hα was not observed.
* = Ratio values likely have contamination from extended
background emission (Sect. 3.2).
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Global notes:
Note (G1): Additional comments as follows:
Cont = non-PMS contaminants discussed in Sect. 4
Dubious = one of 13 sources described in Appendix A with no detected
Hα emission and little IR excess. These stars have a less
secure YSO nature than the other sources.
unclB[e] = one of the four sources identified as of a FS CMa (unclassified
B[e]) nature (see Appendix A)
Young = one of the four sources which are younger than previously known
stars of a similar mass (see Appendix A)
T Tau = the source is inconsistent with M>1.5M☉ and hence
it likely belongs to the T Tauri regime
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Acknowledgements:
Miguel Vioque, miguel.vioque(at)alma.cl
References:
Vioque et al., 2020, PhD thesis University of Leeds
(End) Patricia Vannier [CDS] 09-May-2022