New Low-Mass Members of the Taurus Star-forming Region

By K. Luhman, C. Briceño, J. Stauffer, L. Hartmann, D. B. Navascues, N. Caldwell. 2003

148 citations recorded by the source corpus.

Briceño et al. recently used optical imaging, data from the Two-Micron All-Sky Survey (2MASS), and follow-up spectroscopy to search for young low-mass stars and brown dwarfs in 8 deg2 of the Taurus star-forming region. By the end of that study, there remained candidate members of Taurus that lacked the spectroscopic observations needed to measure spectral types and determine membership. In this work, we have obtained spectroscopy of the 22 candidates that have AV ≤ 8, from which we find six new Taurus members with spectral types of M2.75 through M9. The new M9 source has the second latest spectral type of the known members of Taurus (~0.02 M☉). Its spectrum contains extremely strong emission in Hα (Wλ ~ 950 Å), as well as emission in He I 6678 Å and the Ca II IR triplet. This is the least massive object known to exhibit emission in He I and Ca II, which together with the strong Hα are suggestive of intense accretion.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/c1b5caded4f035df46ad005410327c58014039f8

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Citations in the corpus

The Spectroscopically Determined Substellar Mass Function of the Orion Nebula Cluster (2004, background): “Similar arguments have been put forth by Luhman et al. (2003b) to explain low-lying stars on the HR diagram of IC 348.”
On the Evolutionary Status of Class I Stars and Herbig-Haro Energy Sources in Taurus-Auriga (2004, background): “The now well-established populations of low-mass stars and brown dwarfs in Taurus (e.g., Briceño et al. 1998, 2002; Martı́n et al. 2001; Luhman et al. 2003) are in general too faint to have been detected in previous mid- and far-infrared surveys (e.g., IRAS ), from which spectral indices and…”
THE PALOMAR/KECK ADAPTIVE OPTICS SURVEY OF YOUNG SOLAR ANALOGS: EVIDENCE FOR A UNIVERSAL COMPANION MASS FUNCTION (2008, result): “…β = 0) parallels results from spectroscopic studies of the initial mass function (IMF) of low-mass objects in star-forming regions (Briceño et al. 2002; Luhman et al. 2003a,b; Slesnick et al. 2004; Luhman et al. 2004), which are broadly consistent with α ∼ 0 (where α is the exponent in dN/dM ∝…”
A Census of the Young Cluster IC 348 (2003, methodology): “In comparison, the similarly derived IMF for Taurus from Luhman et al. (2003a) rises quickly to a peak near 0.8 M and steadily declines to lower masses.”
YOUNG L DWARFS IDENTIFIED IN THE FIELD: A PRELIMINARY LOW-GRAVITY, OPTICAL SPECTRAL SEQUENCE FROM L0 TO L5 (2008, background): “Unfortunately, nearinfrared data of young objects systematically yield later spectral types than optical spectra (Luhman et al. 2003b).”
The Formation and Early Evolution of Low-Mass Stars and Brown Dwarfs (2012, methodology): “When combined with the temperature scale from Luhman et al. (2003b) and the 1 Myr isochrone of Baraffe et al. (1998), this classification implies a mass of ∼ 0.2 M⊙, which falls between the dynamical masses of the components as it should.”
A Census of the Chamaeleon I Star-forming Region (2004, methodology): “After considering the available sets of models, Luhman et al. (2003b) concluded that those of Palla & Stahler (1999) for M/M ⊙ > 1 and Baraffe et al. (1998) and Chabrier et al. (2000) for M/M ⊙ ≤ 1 provided the best agreement with observational constraints.”
MAPPING THE SHORES OF THE BROWN DWARF DESERT. II. MULTIPLE STAR FORMATION IN TAURUS–AURIGA (2011, methodology): “This procedure combines the 2 Myr isochrone of Baraffe et al. (1998) with the temperature scales of Schmidt-Kaler (1982) and Luhman et al. (2003) to directly convert spectral types to masses.”
The importance of radiative feedback for the stellar initial mass function (2008, result): “The IMF of the Taurus cloud (Luhman et al. 2003) is also similar to the IMFs presented in Figure 7 in the sense that they both seem to contain an excess of∼ 1 M stars when compared to parameterisations of a universal IMF.”
New Brown Dwarfs and an Updated Initial Mass Function in Taurus (2004, methodology): “While reviewing the available observational constraints for their predictions, they suggested that the observed IMFs in Taurus and denser clusters are the same, citing Kenyon & Hartmann (1995) for the Taurus data.”
THE DISK POPULATION OF THE TAURUS STAR-FORMING REGION (2009, methodology): “…al. 1999; Mart́ın 2000; Mart́ın et al. 2001; Steffen et al. 2001; White & Ghez 2001; Hartigan & Kenyon 2003; Muzerolle et al. 2003; Walter et al. 2003; White & Basri 2003; Luhman 2004b, 2006; Luhman et al. 2003a, 2006, 2009a,b; Guieu et al. 2006; Slesnick et al. 2006; Beck 2007; Prato et al. 2009).”
The Stellar Population of the Chamaeleon I Star-forming Region (2007, methodology): “Thus, the characteris- tic mass of the IMF exhibits no noticeable variation among Orion, Chamaeleon, and Perseus.”
The T Tauri Phase Down to Nearly Planetary Masses: Echelle Spectra of 82 Very Low Mass Stars and Brown Dwarfs (2005, methodology): “Luhman et al. (2003b) compare their IC 348 sample to that of the Brinceño et al. (2002) low-mass sample in Taurus and show that the Taurus sources appear slightly younger overall than the IC 348 ones: they ascribe a median age of 1 Myr to Taurus and 2 Myr to IC 348.”
A Spitzer Census of the IC 348 Nebula (2007, methodology): “4 Steward Observatory, University of Arizona Tucson, AZ 85712; jamesm@as.arizona.edu, eyoung@as.arizona.edu big 1998), near-infrared (Lada & Lada 1995; Muench et al. 2003, hereafter, LL95 and M03 respectively) and spectroscopic surveys (Luhman et al. 1998b; Luhman 1999; Luhman et al. 2003b, 2005a).”
THE HAWAII INFRARED PARALLAX PROGRAM. II. YOUNG ULTRACOOL FIELD DWARFS (2016, background): “The absolute magnitudes of this object derived from our CFHT parallax are ≈5 mag brighter than the field dwarf sequence and comparable to very young (.3 Myr old) mid-M dwarfs in the Taurus star-forming region (e.g. Luhman et al. 2003).”
AN INFRARED/X-RAY SURVEY FOR NEW MEMBERS OF THE TAURUS STAR-FORMING REGION (2009, methodology): “This variation in the IMF is illustrated in Figure 12, where we include mass functions for IC 348 and Chamaeleon I that were derived in the same manner as our measurement for Taurus (Luhman et al. 2003b; Luhman 2007).”