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The Taurus Molecular Cloud: Multiwavelength Surveys with XMM-Newton, the Spitzer Space Telescope, and the Canada-France-Hawaii Telescope*

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The Taurus Molecular Cloud: Multiwavelength Surveys with XMM-Newton, the Spitzer Space Telescope, and the Canada-France-Hawaii Telescope* Güdel et al.: Multiwavelength Surveys of the Taurus Molecular Cloud 329 The Taurus Molecular Cloud: Multiwavelength Surveys with XMM-Newton, the Spitzer Space Telescope, and the Canada-France-Hawaii Telescope* Manuel Güdel Paul Scherrer Institut Deborah L. Padgett California Institute of Technology Catherine Dougados Laboratoire d’Astrophysique de Grenoble The Taurus Molecular Cloud (TMC) ranks among the nearest and best-studied low-mass star-formation regions. It contains numerous prototypical examples of deeply embedded pro- tostars with massive disks and outflows, classical and weak-lined T Tauri stars, jets and Herbig- Haro objects, and a growing number of confirmed brown dwarfs. Star formation is ongoing, and the cloud covers all stages of pre-main-sequence stellar evolution. We have initiated com- prehensive surveys of the TMC, including in particular (1) a deep X-ray survey of about 5 deg2 with XMM-Newton; (2) a near- to mid-infrared photometric survey of ≈30 deg2 with the Spitzer Space Telescope, mapping the entire cloud in all available photometric bands; and (3) a deep optical survey using the Canada-France-Hawaii Telescope. Each wavelength regime contrib- utes to the understanding of different aspects of young stellar systems. XMM-Newton and Spitzer mapping of the central TMC is a real breakthrough in disk characterization, offering the most detailed studies of correlations between disk properties and high-energy magnetic proc- esses in any low-mass star-forming region, extending also to brown dwarfs in which disk physics is largely unexplored. The optical data critically complements the other two surveys by allow- ing clear source identification with 0.8" resolution, identifying substellar candidates, and, when combined with NIR data, providing the wavelength baseline to probe NIR excess emission. We report results and correlation studies from these surveys. In particular, we address the physi- cal interpretation of our new X-ray data, discuss the entire young stellar population from em- bedded protostars to weak-lined T Tau stars and their environment, and present new results on the low-mass population of the TMC, including young brown dwarfs. 1. INTRODUCTION (Spitzer) now obtain detailed infrared photometry and spec- troscopy with diagnostics for disk structure and chemical In a modern picture of star formation, complex feedback composition of the gas and dust in the circumstellar envi- loops regulate mass accretion processes, the ejection of jets ronment. Furthermore, optical surveys have reached a sen- and outflows, and the chemical and physical evolution of sitivity and area coverage with which a detailed census of disk material destined to form planets. Observations in X- the substellar population has become possible. rays with Chandra and XMM-Newton penetrate dense mo- Near- to far-infrared (IR) emission originates predomi- lecular envelopes, revealing an environment exposed to high nantly in the dusty environment of the forming stars, either levels of X-ray radiation. In a complementary manner, ob- in contracting gaseous envelopes or in circumstellar disks. servations in the infrared with the Spitzer Space Telescope IR excess (relative to the photospheric contributions) has been successfully used to model disk geometry, the structure *With significant contributions from Lori Allen (CfA), Marc Audard of the envelope, and also the composition and structure of (Columbia University), Jerôme Bouvier (Grenoble), Kevin Briggs (PSI), dust grains (d’Alessio et al., 1999). Sean Carey (Caltech), Elena Franciosini (Palermo), Misato Fukagawa X-rays play a crucial role in studies of star formation, (Caltech), Nicolas Grosso (Grenoble), Sylvain Guieu (Grenoble), Dean both physically and diagnostically. They may be generated Hines (Space Science Institute), Tracy Huard (CfA), Eugene Magnier (IfA at various locations in young stellar systems, such as in a Honolulu), Eduardo Martín (IAC, Spain), François Ménard (Grenoble), Jean-Louis Monin (Grenoble), Alberto Noriega-Crespo (Caltech), Fran- “solar-like” coronal/magnetospheric environment, in shocks cesco Palla (Florence), Luisa Rebull (Caltech), Luigi Scelsi (Palermo), forming in accretion funnel flows (e.g., Kastner et al., 2002), Alessandra Telleschi (PSI), and Susan Terebey (CalStateLA). or in jets and Herbig-Haro flows (e.g., Pravdo et al., 2001; 329 330 Protostars and Planets V Bally et al., 2003; Güdel et al., 2005). By ionizing circum- tionary speeds for different objects. The infall timescale is stellar material, X-rays also determine some of the preva- a few times 105 yr, while the disk phase amounts to a few lent chemistry (Glassgold et al., 2004) while making the times 106 yr. gas accessible to magnetic fields. Ionization of the circum- TMC has also been well-studied at millimeter wave- stellar-disk surface may further drive accretion instabilities lengths, having better high-resolution molecular line maps (Balbus and Hawley, 1991). Many of these X-ray related than any other star-forming region (Onishi et al. 2002). This issues are summarized in the chapter by Feigelson et al., region has been a major site for searches of complex mol- based on recent X-ray observations of star-forming regions. ecules (Kaifu et al., 2004); many molecular transitions have been mapped across a large area, and the results will be 1.1. The Taurus Molecular Cloud Complex interesting to compare with large-scale IR dust maps of the TMC (see Fig. 3 below). The Taurus Molecular Cloud (TMC) has played a fun- In X-rays, TMC has again played a key role in our under- damental role in our understanding of low-mass star for- standing of high-energy processes and circumstellar mag- mation. At a distance around 140 pc (e.g., Loinard et al., netic fields around pre-main-sequence stars. Among the key 2005; Kenyon et al., 1994), it is one of the nearest star-for- surveys are those by Feigelson et al. (1987), Walter et al. mation regions (SFR) and reveals characteristics that make (1988), Bouvier (1990), Strom et al. (1990), Damiani et al. it ideal for detailed physical studies. One of the most no- (1995), and Damiani and Micela (1995) based on Einstein table properties of the TMC in this regard is its structure in Observatory observations, and the work by Strom and Strom which several loosely associated but otherwise rather iso- (1994), Neuhäuser et al. (1995), and Stelzer and Neuhäuser lated molecular cores each produce one or only a few low- (2001) based on ROSAT. These surveys have characterized mass stars, different from the much denser cores in ρ Oph the overall luminosity behavior of TTS, indicated a depen- or in Orion. TMC features a low stellar density of only 1– dence of X-ray activity on rotation, and partly suggested X- 10 stars pc–2 (e.g., Gómez et al., 1993). Strong mutual in- ray differences between CTTS and WTTS. fluence due to outflows, jets, or gravitational effects are therefore minimized. Furthermore, most stars in TMC are 1.2. Is the Taurus Molecular Cloud Anomalous? subject to relatively modest extinction, providing access to a broad spectrum of stars at all evolutionary stages from Although TMC has been regarded, together with the Class 0 sources to near-zero-age main-sequence T Tau stars. ρ Oph dark cloud, as the prototypical low-mass star-forming TMC has also become of central interest for the study of region, a few apparent peculiarities should be mentioned. substellar objects, in particular brown dwarfs (BD), with TMC contains an anomalously large fraction of binaries regard to their evolutionary history and their spatial distri- (Ghez et al., 1993) compared with other SFRs (e.g., Orion) bution and dispersal (Reipurth and Clarke, 2001; Briceño or with field stars. In TMC, about two-thirds of all members et al., 2002). are bound in multiple systems, with an average separation TMC has figured prominently in star-formation studies of about 0.3" (e.g., Leinert et al., 1993; Mathieu, 1994; at all wavelengths. It has provided the best-characterized Simon et al., 1995; Duchêne et al., 1999; White and Ghez, sample of classical and weak-lined T Tau stars [CTTS and 2001; Hartigan and Kenyon, 2003). Also, TMC cloud cores WTTS, respectively, or “Class II” and “Class III” objects are comparatively small and low-mass when compared with (Kenyon and Hartmann, 1995)]; most of our current pic- cores in Orion or Perseus (Kun, 1998). ture of low-density star formation is indeed based on IRAS TMC has also been found to be deficient of lowest-mass studies of TMC (Beichman et al., 1986; Myers et al., 1987; stars and BDs, with a mass distribution significantly enriched Strom et al., 1989; Kenyon et al., 1990; Weaver and Jones, in 0.5–1 M stars, compared to Orion samples (Briceño et 1992; Kenyon and Hartmann, 1995). Among the key results al., 2002). The formation of BDs may simply be different in from TMC studies as listed in Kenyon and Hartmann (1995) the low-density environment of TMC compared to the dense figure the following: (1) More than 50% of the TMC objects packing of stars in Orion. have IR excess beyond the photospheric contribution, cor- Furthermore, for reasons very poorly understood, TMC relating with other activity indicators (Hα, UV excess, etc.) differs from other SFRs significantly with regard to X-ray and indicating the presence of warm circumstellar material properties. Whereas no X-ray activity-rotation correlation predominantly in the form of envelopes for Class I proto- (analogous to that in main-sequence stars) is found for sam- stars and circumstellar disks for Class II stars. (2) Class III ples in the Orion star-forming regions, perhaps suggesting sources (mostly to be identified with WTTS) are distinctly that all stars are in a saturated state (Flaccomio et al., 2003a; different from lower classes by not revealing optically thick Preibisch et al., 2005a), the X-ray activity in TMC stars has disks or signatures of accretion.
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