A Survey and Analysis of Spitzer Infrared Spectrograph Spectra of T Tauri Stars in Taurus

By E. Furlan, L. Hartmann, N. Calvet, P. D’Alessio, R. Franco-Hernández, W. Forrest, D. Watson, K. Uchida, B. Sargent, J. Green and 13 more. 2006

339 citations recorded by the source corpus.

We present mid-infrared spectra of T Tauri stars in the Taurus star-forming region obtained with the Spitzer Infrared Spectrograph (IRS). For the first time, the 5-36 μm spectra of a large sample of T Tauri stars belonging to the same star-forming region is studied, revealing details of the mid-infrared excess due to dust in circumstellar disks. We analyze common features and differences in the mid-IR spectra based on disk structure, dust grain properties, and the presence of companions. Our analysis encompasses spectral energy distributions from the optical to the far-infrared, a morphological sequence based on the IRS spectra, and spectral indices in IRS wave bands representative of continuum emission. By comparing the observed spectra to a grid of accretion disk models, we infer some basic disk properties for our sample of T Tauri stars and find additional evidence for dust settling.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/1465ebb19ca2e998845efafb5de6a1c506641d64

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In Astronomy and Astrophysics

1. K. Luhman
2. L. Hartmann
3. L. Hillenbrand
4. N. Calvet
5. G. Herczeg
6. Eric Mamajek
7. S. Andrews
8. A. Kraus

Citations in the corpus

• A SPITZER SURVEY OF MID-INFRARED MOLECULAR EMISSION FROM PROTOPLANETARY DISKS. I. DETECTION RATES (2010, background): “This may, to some extent, reflect an intrinsic property of transitional disks, although one canonical transitional disk that is not in our sample — GM Aur — only has a 31µm brightness of ∼ 1 Jy (Furlan et al. 2006).”
• AN OPTICAL SPECTROSCOPIC STUDY OF T TAURI STARS. I. PHOTOSPHERIC PROPERTIES (2014, background): “How disk mass, structure and accretion rate change with age and mass requires accurate spectral typing and luminosity measurements (e.g. Furlan et al. 2006; Sicilia-Aguilar et al. 2010; Oliveira et al. 2013; Andrews et al. 2013).”
• Probing dust grain evolution in IM Lupi's circumstellar disc. Multi-wavelength observations and mo (2008, methodology): “These regions roughly correspond to what is defined as the disc surface in Furlan et al. (2005, 2006) and D’Alessio et al. (2006).”
• Spitzer Observations of the Orion OB1 Association: Disk Census in the Low-Mass Stars (2007, methodology): “…represent the quartiles of disk-bearing stars in Taurus, calculated from the K ½5:8 color in Hartmann et al. (2005) and from the K ½24 color estimated from the median SED slope in Furlan et al. (2006) in the Orionis cluster fromHernández et al. (2007) in 25Orionis and in Ori OB1b from this work.”
• DUST FILTRATION BY PLANET-INDUCED GAP EDGES: IMPLICATIONS FOR TRANSITIONAL DISKS (2012, background): “This choice is based on both our argument in §5.3 (if the dust distribution function is n(s) ∝ s−3 from submicron sizes to 1 mm, 99% of the dust will be in the grains larger than 0.01 mm), and observational constraints (Furlan et al. 2006).”
• Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region (2018, background): “Unlike CoKu Tau 4, IP Tau must have an inner disk to explain the IR excess (Furlan et al. 2006) and active, though very weak, accretion (Gullbring et al. 1998).”
• TRANSITIONAL DISKS AS SIGNPOSTS OF YOUNG, MULTIPLANET SYSTEMS (2011, methodology): “…et al. 1992), a gas/small grain mass ratio of 100 and Equation 10, we see that the total (gas+dust) surface density required for a disk to be vertically optically thin at 13 µm—the spectral index that usually diagnoses flux deficits in transitional disk SEDs (Furlan et al. 2006)—is only 0.2 g cm−2.”
• EXCLUSION OF COSMIC RAYS IN PROTOPLANETARY DISKS: STELLAR AND MAGNETIC EFFECTS (2013, background): “Motivated by the Spitzer inference that small grains are not present in the upper layers of protoplanetary disks, i.e., are settled (Furlan et al. 2006), we have incorporated the UV and X-ray optical effects of dust settling into our model.”
• GIANT PLANET MIGRATION, DISK EVOLUTION, AND THE ORIGIN OF TRANSITIONAL DISKS (2009, methodology): “Najita et al. (2007) identified a sample of 12 transitional disks in the Taurus-Auriga cloud, using 5–30µm data from theSpitzer spectroscopic survey of Furlan et al. (2006).”
• On the Diversity of the Taurus Transitional Disks: UX Tauri A and LkCa 15 (2007, methodology): “When compared to the median SED of Taurus (D’Alessio et al. 1999; Furlan et al. 2006, Fig.”
• TRANSITIONAL AND PRE-TRANSITIONAL DISKS: GAP OPENING BY MULTIPLE PLANETS? (2010, background): “There are a significant number of T Tauri systems in which the disk is optically-thick at a wide range of radii, but which are much more geometrically flat based on their SEDs (e.g., the “group E” systems shown in Figure 7 of Furlan et al. 2006).”
• CRYSTALLINE SILICATES AND DUST PROCESSING IN THE PROTOPLANETARY DISKS OF THE TAURUS YOUNG CLUSTER (2007, methodology): “Second, PAH features at 6.2, 7.7, and 8.6 μm appear in the spectra of more-massive YSOs (e.g., in V892 Tau, AB Aur, and SU Aur; Furlan et al. 2006), and are usually much brighter than the 11–13 μm features, but are weak or absent in the spectrum of UX Tau A. Spectra of members of our sample have…”
• AN INFRARED/X-RAY SURVEY FOR NEW MEMBERS OF THE TAURUS STAR-FORMING REGION (2009, background): “Mid-IR excess emission also was detected toward this star in photometry from IRAS (Harris et al. 1988) and a spectrum from Spitzer (Furlan et al. 2006).”
• Size-sorting dust grains in the surface layers of protoplanetary disks (2008, neutral): “…have been studied in great detail with the Infrared Space Observatory (ISO; e.g. Meeus et al. 2001; Bouwman 2001), with ground-based instruments (van Boekel et al. 2003; Honda et al. 2003) and with the Spitzer Space Telescope (e.g. Apai et al. 2005; Kessler-Silacci et al. 2006; Furlan et al. 2006).”
• THE DISK POPULATION OF THE TAURUS STAR-FORMING REGION (2009, methodology): “Furlan et al. (2006, 2009) detected excess emission longward of 12 µm in an IRS spectrum of V819 Tau.”