Highlights from the XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST)

By M. Güdel, K. Briggs, K. Arzner, M. Audard, J. Bouvier, Eric D. Feigelson, E. Franciosini, A. Glauser, N. Grosso, G. Micela and 23 more. 2006

294 citations recorded by the source corpus.

(abridged:) The XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST) surveys the most populated ~5 square degrees of the Taurus star formation region, using the XMM-Newton X-ray observatory to study the thermal structure, variability, and long-term evolution of hot plasma, to investigate the magnetic dynamo, and to search for new potential members of the association. Many targets are also studied in the optical, and high-resolution X-ray grating spectroscopy has been obtained for selected bright sources. The X-ray spectra have been coherently analyzed with two different thermal models (2-component thermal model, and a continuous emission measure distribution model). We present overall correlations with fundamental stellar parameters that were derived from the previous literature. A few detections from Chandra observations have been added. The present overview paper introduces the project and provides the basic results from the X-ray analysis of all sources detected in the XEST survey.Comprehensive tables summarize the stellar properties of all targets surveyed. The survey goes deeper than previous X-ray surveys of Taurus by about an order of magnitude and for the first time systematically accesses very faint and strongly absorbed TMC objects. We find a detection rate of 85% and 98% for classical and weak-line T Tau stars (CTTS resp. WTTS), and identify about half of the surveyed protostars and brown dwarfs. Overall, 136 out of 169 surveyed stellar systems are detected. We describe an X-ray luminosity vs. mass correlation, discuss the distribution of X-ray-to-bolometric luminosity ratios, and show evidence for lower X-ray luminosities in CTTS compared to WTTS. Detailed analysis (e.g., variability, rotation-activity relations, influence of accretion on X-rays) will be discussed in a series of accompanying papers.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/fd51491f24b663bb1d8c0b6c3d9119a29f5dad1b

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. K. Luhman
2. L. Hillenbrand
3. J. Owen
4. Eric Mamajek
5. L. Hartmann
6. N. Calvet
7. A. Kraus
8. P. R. Allen

In Geophysics

1. Jeroen Tromp
2. J. Owen
3. Yanqin Wu
4. M. Gudel
5. J. Reeves
6. Qinya Liu
7. Dimitri Komatitsch
8. Andreas Fichtner

Citations in the corpus

• Protoplanetary disc evolution and dispersal: the implications of X-ray photoevaporation (2010, methodology): “Therefore, we have used the data for the Taurus cluster (Güdel et al. 2007) and the Orion Nebular cluster (Preibisch et al. 2005) to build cumulative X-ray luminosity functions 1 for the Orion sample functions (XLFs) for all pre-main sequence stars (including both CTTs and WTTs) in the 0.5 to 1 M⊙…”
• A Universal Stellar Initial Mass Function? A critical look at variations in extreme environments (2010, background): “Most recently, Luhman et al. (2009) analyzed Spitzer observations and x–ray data obtained from the XMM satellite (XEST - XMM-Newton Extended Survey of Taurus; Güdel et al. 2007).”
• On the theory of disc photoevaporation (2011, methodology): “While stars with X-ray luminosities <1029 erg s−1 only represent a small fraction ∼5–10 per cent of the population of young stars (Güdel et al. 2007; Owen et al. 2011b), the role of combined FUV/Xray heated flows will certainly be important for these objects if the FUV luminosity continues to…”
• DISCOVERY OF ULTRA-FAST OUTFLOWS IN A SAMPLE OF BROAD-LINE RADIO GALAXIES OBSERVED WITH SUZAKU (2010, result): “This result is also supported by a recent detailed X-ray study of this region that has been performed by the XMM-Newton Extended Survey of the Taurus Molecular Cloud project (Güdel et al. 2007).”
• Radiation-hydrodynamic models of X-ray and EUV photoevaporating protoplanetary discs (2009, result): “…Flaccomio et al. 2009) has been suggested as an observational test for X-ray irradiated discs e.g.(Glassgold et al. 2007; Meijerink et al. 2008; Güdel 2008; Schisano et al. 2009); our calculations open up the possibility of detailed modeling, analogous to that of Alexander (2008b) for the…”
• VLBA Determination of the Distance to Nearby Star-forming Regions. I. The Distance to T Tauri with 0.4% Accuracy (2007, background): “In the meantime, extremely high quality infrared and X-ray surveys of many star-forming regions are being obtained (e.g., Evans et al. 2003; Güdel et al. 2007), and their potential cannot be fully exploited because of the unavailability of good distance estimates.”
• VLBA Determination of the Distance to Nearby Star-forming Regions. II. Hubble 4 and HDE 283572 in Taurus (2007, methodology): “It was detected in VLBI experiments, with a flux of a few millijanskys by Phillips et al. (1991), and is also an X-ray source (Güdel et al. 2007).”
• X-ray spectroscopy of stars (2009, methodology): “A likely origin of these very soft X-rays isthe base of the jet(Güdel et al, 2007c), suggested by i) the unusually soft emission compatible with thejet spectrum, ii) the lowNH values, and iii) the explicit evidence of jets in CHANDRA imaging (Güdel et al, 2008).”
• The Sun in Time: Activity and Environment (2007, background): “Somewhat perplexingly, the analysis of the Taurus sample of embedded objects reveals very little statistical difference between Class I and CTTS objects in Taurus, for example with respect to rotation rates, accretion rates, bolometric luminosities, spectral classes, and disk masses, providing evide”
• DUST AND GAS IN THE DISK OF HL TAURI: SURFACE DENSITY, DUST SETTLING, AND DUST-TO-GAS RATIO (2015, result): “…not formal fits, the high gas velocities and shape of these PV diagrams suggest that the stellar mass is closer to ∼ 1.7 M ; this compares with the estimates of 1.2 M based on HR tracks (Güdel et al. 2007) and 1.3 M based on the approximate extent and width of the HCO+ emission line in ALMA15.”
• X-ray emission from T Tauri stars and the role of accretion: inferences from the XMM-Newton extended survey of the Taurus molecular cloud (2006, methodology): “In total, 45 out of the 159 stellar systems surveyed by XMM-Newton are multiple (Güdel et al. 2007a).”
• KEPLER PLANETS: A TALE OF EVAPORATION (2013, background): “However, the total received X-ray flux at a fixed bolometric flux (so fixed equilibrium temperature) can vary greatly, with late-type stars being significantly more X-ray luminous when integrated over Gyr time-scales (Güdel 2004; Güdel et al. 2007; Jackson et al. 2012).”
• THE TAURUS SPITZER SURVEY: NEW CANDIDATE TAURUS MEMBERS SELECTED USING SENSITIVE MID-INFRARED PHOTOMETRY (2009, methodology): “We note that many of the X-ray detected XEST sources are likely background galaxies (see Güdel et al. 2007) and that XEST included regions not covered by our map, such as L1551.”
• THE DISK POPULATION OF THE TAURUS STAR-FORMING REGION (2009, methodology): “For this sample, we have selected all known members within the fields observed during the XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST, Güdel et al. 2007).”
• AN INFRARED/X-RAY SURVEY FOR NEW MEMBERS OF THE TAURUS STAR-FORMING REGION (2009, methodology): “The unique capabilities of these facilities have been applied to the Taurus star-forming region through the Taurus Spitzer Legacy Survey (D. Padgett, in preparation) and the XMM-Newton Extended Survey of the Taurus Molecular Cloud (XEST, Güdel et al. 2007).”
• Dynamics of Protoplanetary Disks (2010, background): “In the Taurus star-forming region, for example, Güdel et al. (2007) find that the X-ray luminosity of detected sources scales with the stellar mass as, log(LX/erg s −1) = 1.54 log(M∗/M ) + 30.31, (30) for masses in the range 0.1 M ∼< M∗ < 2 M .”