IGRINS and the Evolution of Young Stars and Their Disks

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IGRINS and the Evolution of Young Stars and Their Disks IGRINS and the evolution of young stars and their disks Gregory J. Herczeg (沈雷歌, Shěn Léigē ) Kavli Institute for Astronomy and Astrophysics, Peking University Pre-main sequence stellar evolution Protostar Classical T Tauri star Weak-line T Tauri star Low mass stars Stellar Growth (BAE Jaehan+2014) New JCMT Transient Survey PIs Herczeg, Johnstone ALMA HL Tau (disk+remnant envelope) IRS 48: full gas ring revealed Dust trap in a transition disks Cycle 2 data Band 9 (van der Marel PI) (van der Marel+2013, 2015) Dust: trapped at 50 AU CO 6-5: symmetric 0.44 mm cont 13CO 6-5 Comet/KBO factory? Van der Marel et al. in prep - Dust trap optically thick, blocking some of 13CO emission? - Kinematics of gas around dust trap can test vortex model (Proto?)-planet detection in a disk hole 3 Myr old Kraus & Ireland 2012: see also Quanz+2014, 2015 Disk lifetimes Planet formation Lifetimes of Envelope Disk lifetimes Planet formation Lifetimes of Envelope Veiling: emission from disk/accretion weakens photospheric lines Optical spectra of TW Hya on different days Near-IR: disk wall variability (e.g., Ingleby+2015; Stauffer+2015) Emission lines may fill in absorption lines (TW Hya; Herczeg+ in prep) Spectral types and extinctions in Taurus (Herczeg & Hillenbrand 2014) Accretion, extinction, and veiling simultaneously on 283 stars 1 mag discrepancy with near-IR extinctions (e.g.Furlan+) Recalibrate SpT-Temperature conversion based on BT-Settl models (but see Tottle & Mohanty for caveats) 14 Changes in stellar parameters: DM Tau Herczeg Previously M1: M=0.68 Msun, age = 11 Myr (old Baraffe models) Classified as M3: M=0.38 Msun, age = 3.5 Myr Fig. 16.— The red optical spectra of DM Tau (top, M2.9) and TW Hya (bottom, M0.6), after subtracting a flat accretion continuum. DM Tau is classified as an M2.9 while TW Hya is classified as M0.6. Previous spectral type measurements are inconsistent with the observed spectra. UScoCTIO 33 was originally identified as a possible 4.3.2. DM Tau member of the Upper Scorpius OB Association in a pho- tometric survey by Ardila et al. (2000). A spectroscopic The literature spectral type of M1 for DM Tau traces survey by Preibisch et al. (2002) confirmed membership, back to Cohen & Kuhi (1979). Despite significant in- classified the star as M3, and found strong Hα emission terest as the host of a transition disk (e.g. Calvet et al. indicative of accretion. 2005), its spectral type has not been reassessed using Figure 15 shows our Keck spectrum of UScoCTIO modern techniques. 33 compared with M3 and M4.5 stars with a veiling Fig. 16 shows the veiling-corrected DM Tau spectrum r7525=0.0 and 0.25. If the veiling is 0, the red spectrum 29 Dec. 2008, compared with M2, M2.9, and M4 spectra. is best classified as an M3 spectral type, with only small The veiling is calculated from the depth of the Ca I 4227 inconsistencies between the template and the spectrum. A˚ line. The veiling r7510 =0.17 leads to SpT of M2.9 However, the M3 template spectrum is much weaker than and AV =0.08. If the composite photospheric+accretion the observed blue emission. spectrum is not constrained by a good fit to the Ca I The veiling r7525=0.25 is calculated from the depth λ4227 line, then r7510 could range from 0.09, with SpT of the Ca I λ4227 line. Subtracting this accretion con- M2.7 and AV = −0.20, to 0.31, with SpT M3.4 and AV = tinuum off of the observed spectrum yields photospheric 0.50. In this case, the extinction actually increases with lines that are deeper than the uncorrected observation. later spectral type because the veiling has increased. If The consequent M4.5 spectral type with veiling improves the blue side is ignored entirely, then a veiling of r7510 =0 the fit to the red and blue spectra. would yield M2.5 and AV =0.06 while an upper limit With an M4.5 SpT and Baraffe et al. (2003) pre-main on veiling of r7510 =0.39 would yield M4.1 and AV = sequence tracks, the mass and age are 0.16 M⊙ and 6.5 −0.06. In these latter cases, the resulting red spectrum Myr, respectively, wheareas the M3 SpT yields 0.31 M⊙ looks reasonable. The uncertainties in SpT and veiling and 26 Myr. are about half the size of these ranges when using the blue and red spectra together. Even with the blue+red LkCa 4 (WTTS) Spotted High resolution optical, Donati+2014 Low-res red optical, Herczeg+2014 Age spreads of young cluster (see also Soderblom+2014) Observational uncertainties? Accretion histories? Real age spread Offsets between empirical and model isochrones lead to mass-dependent ages Baraffe+1998 isochrones mixing length 1.0 Herczeg & Hillenbrand 2015 New tracks fit much better! (Baraffe+2015; Feiden+ in prep) Baraffe+2015 isochrones Don’t age-date individual objects, but especially those at <3300 K (M3)! Still offsets at <3500 K; no assessment of >5000 K Consistent age estimates Upper Sco: young stars are 4 Myr Pecaut & Mamajek: intermediate/high mass stars are 11 Myr EmpiricalIsochronesforLowMassStars 13 TABLE 5 Consistent Sets of Ages (in Myr) Estimated from a Single ModelandTemperaturea Stellar DM97 Tognelli BCAH-1.0 Feiden BHAC-2015 Li Depl.b Association d (pc) log L4200/L⊙ 3400 K 4200 4200 K 3800 3800 Age Upper Sco 145 ± 10 −0.23 ± 0.06 1.6 ± 0.24.6 ± 1.19.7 ± 1.9 3.8 ± 1.03.8 ± 1.0 – ϵ Cha 111 ± 5 −0.28 ± 0.06 1.9 ± 0.35.6 ± 1.411.3 ± 2.1 4.7 ± 1.24.7 ± 1.2 – η Cha 94 ± 5 −0.32 ± 0.05 2.1 ± 0.36.6 ± 1.312.7 ± 2.1 5.5 ± 1.35.5 ± 1.3 – TWA (57) −0.40 ± 0.04 2.7 ± 0.49.0 ± 1.516.5 ± 2.1 7.9 ± 1.48.1 ± 1.4 – BPMG (30) −0.65 ± 0.04 6.1 ± 0.724± 436± 5 23 ± 422± 4 25 ± 4 Tuc Hor (51) −0.72 ± 0.02 7.7 ± 0.532± 344± 3 30 ± 329± 3 40 ± 4 aFor models that produce younger, intermediate, and older ages, and separately for the Feiden and BHAC-15 tracks. These sets of ages are calculated from a single model at a single Teff ,appliedconsistentlytoeachassociation. bLi depletion boundary ages, see text for details. improved match between predicted and observed stellar Figure 12 and Table 5 compares the Li depletion loci. boundary ages to the isochronal ages estimated here from Ultimately, some model improvements are necessary the different model tracks. For 3800 K stars, the Siess, so that the evolution of radius and temperature bet- Tognelli, Dotter, and BCAH-1.9, BHAC-2015, and Fei- ter reflects the observational constraints of young stellar den models predict ages that are roughly consistent with associations. One of these improvements, the inclusion the Li depletion boundary ages, within the uncertain- of magnetic fields in the Dartmouth models, provides a ties. Ages from PARSEC and BCAH-1.0 are too old and much better match to empirical isochrones. Age com- DM97 are too young, while Tognelli, Dotter, and BCAH parisons between clusters are accurate only when com- models at 3400 K yield ages that are too young. Apply- pared over specific temperature ranges where the model ing the DM97 models yield especially young ages, likely and empirical isochrones match. The magnetic Feiden because the isochrones of low-mass stars have tempera- models currently offer the best set of pre-main sequence tures that are initially too high (see description in §2.5). tracks for relative age estimates, although mismatches at Both the Feiden and BHAC-2015 models have similar < 3500 K still lead to temperature-dependent ages. The isochrones that yield remarkably similar ages. empirical isochrones derived in this paper offer a method When applied consistently, the Li depletion boundary to place stars of different temperatures on the same age ages for the Tuc-Hor and β Pic Moving Group imply a scale, albeit with some uncertainty introduced by the ∼ 5 Myr old age for low mass stars in the Upper Sco possible temporal evolution of the isochronal slopes. OB Association, younger than the 11 Myr age measured Table 5 lists sets ages for each cluster based on a con- from intermediate and high mass stars by Pecaut et al. sistent application of a single model family at a single (2012). The 11 Myr age of Upper Sco would require ages stellar temperature. The ages are selected from models of ∼ 40 and 55 Myr for the β Pic and Tuc-Hor Moving that produce young, intermediate, and old ages relative Groups. Either the intermediate mass or low mass age to the average model. Uncertainties in these ages are (based on Li depletion boundary ages of older associa- calculated from the statistical uncertainties in the fits, tions) of the Upper Sco OB Association is incorrect, or as listed in Table 48, and an estimate for the systematic the target selection of one of the samples is biased. uncertainty in the median distance of the η Cha, ϵ Cha, Errors in ages may be caused by either errors in the and Upper Sco OB Associations. birthline or in the contraction rates. A bulk subtraction The reasonableness of these isochronal ages are of 5 Myr to intermediate mass isochrones would shift the testable by comparison to Li depletion boundary ages9. intermediate mass isochrones sufficiently for Upper Sco The Tuc-Hor Moving Group has a Li depletion bound- and would not cause any significant discrepancy with the ary age of 41 ± 2 Myr from the BCAH-1.0 evolutionary Li depletion age of the β Pic Moving Group.
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