IRAC Observations of Taurus Pre-Main-Sequence Stars

By L. Hartmann, S. Megeath, L. Allen, K. Luhman, N. Calvet, P. D’Alessio, R. Franco-Hernández, G. Fazio. 2005

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We present infrared photometry obtained with the IRAC camera on the Spitzer Space Telescope of a sample of 82 pre-main-sequence stars and brown dwarfs in the Taurus star-forming region. We find a clear separation in some IRAC color-color diagrams between objects with and without disks. A few "transition" objects are noted, which correspond to systems in which the inner disk has been evacuated of small dust. Separating pure disk systems from objects with remnant protostellar envelopes is more difficult at IRAC wavelengths, especially for objects with infall at low rates and large angular momenta. Our results generally confirm the IRAC color classification scheme used in previous papers by Allen et al. and Megeath et al. to distinguish between protostars, T Tauri stars with disks, and young stars without (inner) disks. The observed IRAC colors are in good agreement with recent improved disk models, and in general accord with models for protostellar envelopes derived from analyzing a larger wavelength region. We also comment on a few Taurus objects of special interest. Our results should be useful for interpreting IRAC results in other, less well studied star-forming regions.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/ee0190116fba8823017c49b86e58d5b81c29490c

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Citations in the corpus

Interpreting Spectral Energy Distributions from Young Stellar Objects. II. Fitting Observed SEDs Using a Large Grid of Precomputed Models (2006, methodology): “In addition, we have measured the IRAC fluxes for the sources not presented in Hartmann et al. (2005) or Luhman et al. (2006), and re-measured the IRAC fluxes of RY Tau and DG Tau, which are saturated in all bands.”
THE TW Hya DISK AT 870 μm: COMPARISON OF CO AND DUST RADIAL STRUCTURES (2011, methodology): “In the thermal infrared, Spitzer flux densities measured by Hartmann et al. (2005) and Low et al. (2005) were supplemented with IRAS and Herschel data (Weaver & Jones 1992; Thi et al. 2010).”
Interpreting Spectral Energy Distributions from Young Stellar Objects. I. A Grid of 200,000 YSO Model SEDs (2006, methodology): “As shown by Hartmann et al. (2005), this analysis is appropriate for the Taurus star formation region where most sources have stellar temperatures ranging from 3, 000K to 5, 000K (Kenyon & Hartmann 1995).”
Star and Protoplanetary Disk Properties in Orion's Suburbs (2009, background): “Many young stars in clusters with ages from 1 Myr to tens of Myrs have been studied (e.g. Gutermuth et al. 2004; Young et al. 2004; Hartmann et al. 2005; Megeath et al. 2005b; Lada et al. 2006; Sicilia-Aguilar et al. 2006a, 2008; Hernández et al. 2006; Dahm & Hillenbrand 2007; Hernández et al.…”
Dust dynamics during protoplanetary disc clearing (2007, background): “…excess, arising from the reprocessing of stellar radiation by warm dust in the inner disc disc (Kenyon & Hartmann 1995; Haisch, Lada & Lada 2001; Hartmann et al. 2005), accretion signatures such as line emission and ultraviolet excess (Hartigan, Edwards & Ghandour 1995; Calvet & Gullbring 1998;…”
The Spitzer c2d Survey of Weak-Line T Tauri Stars. II. New Constraints on the Timescale for Planet Building (2007, background): “Systems with λturn−off ≤ 2.0 µm show some excess in the near-IR JHK bands and are probably actively accreting (see e.g. Hartmann et al. 2005 and Muzerolle et al. 2003).”
THE DISK POPULATION OF THE TAURUS STAR-FORMING REGION (2009, methodology): “However, while class III stars are easily distinguished from less evolved systems, some class I and class II sources can exhibit similar SEDs in the Spitzer bands (Hartmann et al. 2005).”
Spitzer Observations of IC 348: The Disk Population at 2-3 Million Years (2005, background): “…over an interesting range of wavelengths, extending well into the mid-infrared wavelength bands in reasonable amounts of observing time (e.g., Hartmann et al. 2005; SiciliaAguilar et al. 2006).Mid-infraredwavelengths are ideal for studying disks, because these wavelengths are well removed…”
VOSA: Virtual Observatory SED Analyzer. An application to the Collinder 69 open cluster (2008, methodology): “Barrado y Navascués et al. (2007b) studied in detail the Spitzer/IRAC data of the candidates, and based on the criteria developed by Allen et al. (2004) and Hartmann et al. (2005) derived a fraction of members with disks of 25% and 40% for the stellar and substellar population of C69, respectively.”
A Submillimeter View of Circumstellar Dust Disks in ρ Ophiuchi (2007, methodology): “The infrared photometry of Taurus sources utilized for this same purpose in Paper I was supplemented with Spitzer Space Telescope photometry from Hartmann et al. (2005) and Luhman et al. (2006).”
THE TAURUS SPITZER SURVEY: NEW CANDIDATE TAURUS MEMBERS SELECTED USING SENSITIVE MID-INFRARED PHOTOMETRY (2009, background): “Flux densities here are those from Hartmann et al. (2005); since their observations have more redundancy at IRAC bands, they are able to obtain reliable flux densities for this object at IRAC bands.”
A Spitzer Space Telescope Study of Disks in the Young σ Orionis Cluster (2007, background): “Recent Spitzer results for the young stellar clusters NGC 7129 (Gutermuth et al. 2004), Taurus (Hartmann et al. 2005), Chameleonis (Megeath et al. 2005a), Tr 37 and NGC 7160 (Sicilia-Aguilar et al. 2006), IC 348 (Lada et al. 2006), and Upper Scorpius (Carpenter et al. 2006) have been included in thi”
HIGH- AND INTERMEDIATE-MASS YOUNG STELLAR OBJECTS IN THE LARGE MAGELLANIC CLOUD (2009, background): “…of low-mass stars can be studied in great detail in nearby star-forming regions (e.g., Taurus-Auriga Molecular Cloud; Kenyon & Hartmann 1995; Hartmann et al. 2005), but the formation of stars more massive than a few solar masses cannot be studied easily because such 1 Visiting astronomer,…”
The Spitzer c2d Survey of Large, Nearby, Interstellar Clouds. IX. The Serpens YSO Population as Observed with IRAC and MIPS (2007, background): “%) show larger fluxes than the median SED of Taurus.”
WIDE-FIELD INFRARED SURVEY EXPLORER OBSERVATIONS OF THE EVOLUTION OF MASSIVE STAR-FORMING REGIONS (2012, background): “The basis for this scheme is the work of Allen et al. (2004) and Hartmann et al. (2005) who first investigated the distributions of young stars in Spitzer color space.”