J/ApJ/943/49 The IGRINS YSO survey. III. Oph & Upper Sco (Lopez-Valdivia+, 2023)
The IGRINS YSO survey.
III. Stellar parameters of pre-main-sequence stars in Ophiuchus and
Upper Scorpius.
Lopez-Valdivia R., Mace G.N., Han E., Sawczynec E., Hernandez J.,
Prato L., Johns-Krull C.M., Oh H., Lee J.-J., Kraus A., Llama J.,
Jaffe D.T.
<Astrophys. J., 943, 49 (2023)>
=2023ApJ...943...49L 2023ApJ...943...49L
ADC_Keywords: Associations, stellar; YSOs; Spectra, infrared; Spectral types;
Effective temperatures; Magnetic fields; Rotational velocities
Keywords: Fundamental parameters of stars ; Infrared sources ;
Pre-main sequence stars ; High resolution spectroscopy
Abstract:
We used the Immersion GRating Infrared Spectrometer (IGRINS) to
determine fundamental parameters for 61 K- and M-type young stellar
objects (YSOs) located in the Ophiuchus and Upper Scorpius
star-forming regions. We employed synthetic spectra and a Markov chain
Monte Carlo approach to fit specific K-band spectral regions and
determine the photospheric temperature (T), surface gravity (logg),
magnetic field strength (B), projected rotational velocity (vsini),
and K-band veiling (rK). We determined B for ∼46% of our sample.
Stellar parameters were compared to the results from Taurus-Auriga and
the TW Hydrae association presented in Paper I of this series. We
classified all the YSOs in the IGRINS survey with infrared spectral
indices from Two Micron All Sky Survey (2MASS) and Wide-field Infrared
Survey Explorer (WISE) photometry between 2 and 24µm. We found that
Class II YSOs typically have lower logg and vsini, similar B, and
higher K-band veiling than their Class III counterparts. Additionally,
we determined the stellar parameters for a sample of K and M field
stars also observed with IGRINS. We have identified intrinsic
similarities and differences at different evolutionary stages with our
homogeneous determination of stellar parameters in the IGRINS YSO
survey. Considering logg as a proxy for age, we found that the
Ophiuchus and Taurus samples have a similar age. We also find that
Upper Scorpius and TWA YSOs have similar ages, and are more evolved
than Ophiuchus/Taurus YSOs.
Description:
We observed our sample with the Immersion GRating Infrared
Spectrometer (IGRINS) at the McDonald Observatory 2.7m telescope, the
Lowell Discovery Telescope (LDT), and the Gemini South Telescope
between 2014 and 2019. We followed the observing and data reduction
methods as outlined in Paper I (Lopez-Valdivia+ 2021, J/ApJ/921/53).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 148 70 Basic information and results for our Ophiuchus
and Upper Scorpius sample
table3.dat 98 129 *Stellar parameters for Taurus and TWA YSOs
(see Appendix A1)
table4.dat 72 133 Stellar parameters of the K and M field stars
(see Appendix A2)
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Note on table3.dat: We gathered the stellar parameters reported in Paper I
(Lopez-Valdivia+ 2021, J/ApJ/921/53) for the Taurus and TWA YSOs. We
also added the values of AV and computed αKs-W4 in this work
for many of them.
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See also:
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
II/328 : AllWISE Data Release (Cutri+ 2013)
J/ApJ/593/1093 : IC 348 membership (Luhman+, 2003)
J/AJ/130/1733 : Optical spectroscopy of ρ Oph stars (Wilking+, 2005)
J/A+A/460/695 : Search for Associations Containing Young stars (Torres+, 2006)
J/ApJ/712/925 : Transition circumstellar disks in Ophiuchus (Cieza+, 2010)
J/ApJ/709/L114 : Protoplanetary disks in PMS binaries (Duchene, 2010)
J/ApJS/186/111 : Spitzer observations of Taurus members (Luhman+, 2010)
J/ApJS/205/5 : YSO candidates in nearby molecular clouds (Hsieh+, 2013)
J/ApJS/208/9 : Intrinsic colors and temperatures of PMS stars (Pecaut+, 2013)
J/ApJ/786/97 : Photospheric properties of T Tauri stars (Herczeg+, 2014)
J/ApJ/785/47 : Sources around target stars in Upper Sco (Lafreniere+, 2014)
J/ApJS/220/11 : SEDs of Spitzer YSOs in the Gould Belt (Dunham+, 2015)
J/AJ/153/46 : Spectroscopy of candidate members in Taurus (Luhman+, 2017)
J/AJ/156/76 : New young stars and brown dwarfs in Upper Sco (Luhman+, 2018)
J/AJ/155/196 : K2 LCs for members of USco & ρ Oph (Rebull+, 2018)
J/A+A/622/A149 : Vienna survey in Orion. III. (Grossschedl+, 2019)
J/ApJ/879/105 : Effective temp. of low-mass stars (Lopez-Valdivia+, 2019)
J/AJ/159/282 : Membership in Ophiuchus & Upper Sco complex (Esplin+, 2020)
J/AJ/160/44 : Upper Scorpius spectroscopy and photometry (Luhman+, 2020)
J/ApJ/921/53 : IGRINS YSO survey. I. Tau-Aur (Lopez-Valdivia+, 2021)
J/ApJ/923/177 : TESS obs. & rot. periods of T Tauri in Orion (Serna+, 2021)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 A17 --- 2MASS 2MASS identification number
(JHHMMSSss+DDMMSSs)
19- 37 A19 --- Name Alternative name
39- 40 I2 --- Nep [1/10] Number of epochs combined
42- 45 F4.1 mag Ksmag [5.8/10.8] Ks magnitude
47- 51 A5 --- SpT Spectral type
53- 54 A2 --- r_SpT Reference for SpT (1)
56- 59 A4 --- cluster Cluster membership, Oph(iuchus) or USco
(Upper Scorpius)
61- 62 A2 --- r_cluster Reference for cluster (1)
64 A1 --- Bin Binary status (2)
66- 67 A2 --- r_Bin Reference for Bin (1)
69- 72 F4.1 mag Av [0.1/8.6]? Visual extinction
74- 77 F4.1 mag e_Av [0.1/1]? Visual extinction uncertainty
79- 83 F5.2 --- alpha [-2.8/-0.07]? Dereddened infrared index
85- 89 F5.2 --- e_alpha [0.02/0.51]? Dereddened infrared index
uncertainty
91 I1 --- Qual [0/3]? Quality flag (0=good, 1=acceptable) (3)
93- 96 I4 K Teff [3129/4652]? Temperature
98- 100 I3 K e_Teff [100/405]? Temperature uncertainty
102- 106 F5.2 [cm/s2] logg [3.15/4.6]? Surface gravity, log cgs
108- 112 F5.2 [cm/s2] e_logg [0.16/0.7]? Surface gravity uncertainty
114 A1 --- l_B Upper limit flag on B
116- 120 F5.2 0.1T B [0.67/2.7]? Magnetic field strength
122- 126 F5.2 0.1T e_B [0.3/1.1]? Magnetic field strength uncertainty
128- 131 F4.1 km/s vsini [6/35.3]? Projected rotational velocity
133- 136 F4.1 km/s e_vsini [1.8/9]? Projected rotational velocity
uncertainty
138- 142 F5.2 --- rk [0.03/7.5]? K-band veiling
144- 148 F5.2 --- e_rk [0.03/1.4]? K-band veiling uncertainty
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Note (1): References for spectral type, cluster and binarity as follows:
1 = Simon et. al. (1995ApJ...443..625S 1995ApJ...443..625S);
2 = Haisch et al. (2002AJ....124.2841H 2002AJ....124.2841H);
3 = Prato et al. (2003ApJ...584..853P 2003ApJ...584..853P);
4 = Ratzka et al. (2005A&A...437..611R 2005A&A...437..611R);
5 = Wilking et al. (2005, J/AJ/130/1733);
6 = Torres et al. (2006, J/A+A/460/695)
7 = Prato (2007ApJ...657..338P 2007ApJ...657..338P);
8 = Kraus et al. (2008ApJ...679..762K 2008ApJ...679..762K);
9 = Ricci et al. (2010A&A...521A..66R 2010A&A...521A..66R);
10 = Duchene (2010, J/ApJ/709/L114);
11 = Cieza et al. (2010, J/ApJ/712/925);
12 = Hsieh & Lai (2013, J/ApJS/205/5);
13 = Lafreniere et al. (2014, J/ApJ/785/47);
14 = Rebull et al. (2018, J/AJ/155/196);
15 = Luhman et al. (2018, J/AJ/156/76);
16 = Barenfeld et al. (2019ApJ...878...45B 2019ApJ...878...45B);
17 = Esplin & Luhman (2020, J/AJ/159/282);
18 = Luhman & Esplin (2020, J/AJ/160/44);
Note (2): We identified binaries (or multiples) in the YSO sample with a
separation of less than 2". When the separation is greater than 2",
the objects can be observed individually by IGRINS. If the separation
is less than 2", the resultant IGRINS spectrum will contain some flux
from both components. See Section 2.
Note (3): Quality flag as follows:
0 = good (31 occurrences)
1 = acceptable (25 occurrences)
2 = objects with lower/upper limits outside or at the edge of our grid
(5 occurrences)
3 = poor determinations (9 occurrences)
See Section 4.
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 A17 --- 2MASS 2MASS identification number
(JHHMMSSss+DDMMSSs; except TWA 3B)
19- 23 A5 --- SpT Spectral type
25- 27 A3 --- cluster Cluster membership, Tau(rus) or TWA
(TW Hydrae Association)
29- 32 F4.1 mag Av [-0.7/7.2]? Visual extinction
34- 36 F3.1 mag e_Av [0.1/2]? Visual extinction uncertainty
38- 41 F4.1 --- alpha [-2.9/0.2]? Dereddened infrared index
43- 45 F3.1 --- e_alpha [0/0.6]? Dereddened infrared index
uncertainty
47 I1 --- Qual [0/2] Quality flag (0=good, 1=acceptable)
49- 52 I4 K Teff [3203/4606] Temperature
54- 56 I3 K e_Teff [75/437] Temperature uncertainty
58- 61 F4.2 [cm/s2] logg [3.2/4.7] Surface gravity, log cgs
63- 66 F4.2 [cm/s2] e_logg [0.1/0.7] Surface gravity uncertainty
68 A1 --- l_B Limit flag on B
71- 74 F4.2 0.1T B [0.9/3.21] Magnetic field strength
76- 79 F4.2 0.1T e_B [0.26/1]? Magnetic field strength uncertainty
81- 84 F4.1 km/s vsini [4.6/43.7] Projected rotational velocity
86- 88 F3.1 km/s e_vsini [1.7/9.7] Projected rotational velocity
uncertainty
90- 93 F4.2 --- rk [0.02/5.6] K-band veiling
95- 98 F4.2 --- e_rk [0.0/1.1] K-band veiling uncertainty
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Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 23 A23 --- Name Star Name
25- 29 A5 --- SpT Spectral type,
Lopez-Valdivia+ 2019, J/ApJ/879/105
31 I1 --- Qual [0/2] Quality flag (0=good, 1=acceptable)
33- 36 I4 K Teff [3391/4996] Temperature (1)
38- 40 I3 K e_Teff [75/335] Temperature uncertainty
42- 45 F4.2 [cm/s2] logg [3.14/5.5] Surface gravity (1)
47- 50 F4.2 [cm/s2] e_logg [0.13/0.5] Surface gravity uncertainty
52 A1 --- l_B Limit flag on B
55- 58 F4.2 0.1T B [0.04/3.81] Magnetic field strength (1)
60- 63 F4.2 0.1T e_B [0.29/2.07]? Magnetic field strength
uncertainty
65- 68 F4.1 km/s vsini [2.3/45.7] Projected rotational velocity (1)
70- 72 F3.1 km/s e_vsini [1.7/5.6] Projected rotational velocity
uncertainty
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Note (1): The stellar parameters are determined using the same MCMC approach,
but ignoring K-band veiling.
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History:
From electronic version of the journal
References:
Lopez-Valdivia et al. Paper I. 2021ApJ...921...53L 2021ApJ...921...53L Cat. J/ApJ/921/53
Kidder et al. Paper II. 2021ApJ...922...27K 2021ApJ...922...27K
Lopez-Valdivia et al. Paper III. 2023ApJ...943...49L 2023ApJ...943...49L This catalog
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 06-Dec-2024