Imaging the Disk around TW Hydrae with the Submillimeter Array

By C. Qi, P. Ho, D. Wilner, S. Takakuwa, N. Hirano, N. Ohashi, T. Bourke, Qizhou Zhang, G. Blake, M. Hogerheijde and 3 more. 2004

176 citations recorded by the source corpus.

We present ~2''-4'' aperture synthesis observations of the circumstellar disk surrounding the nearby young star TW Hya in the CO J = 2-1 and J = 3-2 lines and associated dust continuum obtained with the partially completed Submillimeter Array. The extent and peak flux of the 230 and 345 GHz dust emission follow closely the predictions of the irradiated accretion disk model of Calvet et al. The resolved molecular line emission extends to a radius of at least 200 AU, the full extent of the disk visible in scattered light, and shows a clear pattern of Keplerian rotation. Comparison of the images with two-dimensional Monte Carlo models constrains the disk inclination angle to 7° ± 1°. The CO emission is optically thick in both lines, and the kinetic temperature in the line formation region is ~20 K. Substantial CO depletion, by an order of magnitude or more from canonical dark cloud values, is required to explain the characteristics of the line emission.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/88db86018d234e1e28b44156555a08f4e2659424

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In Astronomy and Astrophysics

1. S. Andrews
2. D. Wilner
3. T. Birnstiel
4. Jonathan P. Williams
5. C. Dullemond
6. A. Hughes
7. Simon Bruderer
8. C. Qi

Citations in the corpus

• High-Resolution Submillimeter Constraints on Circumstellar Disk Structure (2006, background): “…the auspices of more sophisticated models (e.g., D’Alessio et al. 2001; Calvet et al. 2002) to place ever more detailed constraints on properties like structure and chemistry (Wilner et al. 2003; Qi et al. 2003, 2004, 2006), as well as the signatures of grain growth (e.g., Wilner et al. 2005).”
• Spectroastrometric Imaging of Molecular Gas within Protoplanetary Disk Gaps (2008, background): “The inner disk inclination, if more representative of the companion orbit inclination than the outer disk inclination of 7 ± 1◦ by Qi et al. (2004), places this short period companion in the “brown dwarf desert” (Grether & Lineweaver 2006).”
• A SPATIALLY RESOLVED INNER HOLE IN THE DISK AROUND GM AURIGAE (2009, background): “Sev- eral recent millimeter studies have resolved inner emission cavities for disks with infrared SED deficits through direct imaging observations, e.g. TW Hya (Calvet et al. 2002; Hughes et al. 2007), LkHα 330 (Brown et al. 2007, 2008), and LkCa 15 (Piétu et al. 2007; Espaillat et al. 2008).”
• RINGED SUBSTRUCTURE AND A GAP AT 1 au IN THE NEAREST PROTOPLANETARY DISK (2016, methodology): “Each feature was consistent with the standard geometry inferred from molecular line observations (e.g., Qi et al. 2004; Andrews et al. 2012): the joint constraints suggest an inclination of 7 ± 3◦ and a major axis position angle of 155 ± 12◦.”
• Our astrochemical heritage (2012, background): “below 20 K, molecular freeze-out becomes important and simple species typically found in dark clouds are detected: CO isotopologues with evidence of depletion ([141]; [143]; [362]), CN, HCN, HNC, CS, HCO, C2H and H2CO ([142]; [430]; [418]; [99]), N2H + ([144]), SO ([162]), CS ([145]), DCO ([428]), H”
• Gaps, Rings, and Non-Axisymmetric Structures in Protoplanetary Disks - From Simulations to ALMA Observations (2014, background): “CO gas line observations of circumstellar disks frequently find broadened line profiles that cannot be explained by the thermal velocity of the molecules itself (e.g., Guilloteau & Dutrey 1998; Piétu et al. 2007; Qi et al. 2004; Guilloteau et al. 2012).”
• Measuring turbulence in TW Hydrae with ALMA: methods and limitations (2016, background): “With a near face-on inclination of only i ≈ 7◦ (Qi et al. 2004) and as the nearest protoplanetary disk at d ≈ 54 pc, TW Hya provides the best opportunity to directly detect turbulent broadening as the impact of Keplerian shear for such face-on disks is minimized compared to more inclined systems.”
• Volatile carbon locking and release in protoplanetary disks. A study of TW Hya and HD 100546 (2016, unknown): “The inclination is 7◦ ± 1◦ (Qi et al. 2004; Hughes et al. 2011; Andrews et al. 2012; Rosenfeld et al. 2012).”
• Toward Planetesimals in the Disk around TW Hydrae: 3.5 Centimeter Dust Emission (2005, background): “3 National Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801. et al. 2002) and in thermal emission from dust and trace molecules (Weintraub et al. 1989; Kastner et al. 1997; Qi et al. 2004).”
• THE TW Hya DISK AT 870 μm: COMPARISON OF CO AND DUST RADIAL STRUCTURES (2011, methodology): “Despite its ad- vanced age (∼10Myr; Kastner et al. 1997; Webb et al. 1999), it hosts a massive, gaseous accretion disk with a rich molecular spectrum and strong continuum emission out to centimeter wavelengths (Wilner et al. 2000, 2003, 2005; Qi et al. 2004, 2006, 2008).”
• TW Hydrae: evidence of stellar spots instead of a Hot Jupiter (2008, background): “In the case of TW Hya, we choseR⋆ = 0.9 R⊙ (following SHL08) and an inclination ofi = 7◦, which is the likely inclination of the TW Hya circumstellar disk (Qi et al. 2004).”
• Three Radial Gaps in the Disk of TW Hydrae Imaged with SPHERE (2016, background): “Its disk is seen nearly face-on (i ≈ 7 ◦ Qi et al. 2004) and it is the only such object for which a direct measure of the bulk gas mass could be obtained so far.”
• CHEMICAL PROCESSES IN PROTOPLANETARY DISKS (2010, background): “…systems including TW Hydrae (Kastner et al. 1997; van Zadelhoff et al. 2001; van Dishoeck et al. 2003; Ceccarelli et al. 2004; Thi et al. 2004; Qi et al. 2004, 2006, 2008), DM Tauri (Dutrey et al. 1997; Ceccarelli et al. 2004, 2005; Guilloteau et al. 2006; catherine.walsh@qub.ac.uk Dutrey et…”
• Protoplanetary Disks and Their Evolution (2011, background): “Spectral line observations also determine disk inclinations to our line of sight with high accuracy (e.g., Qi et al. 2004), which is necessary for detailed modeling and characterization of other disk properties.”
• Gas and Dust Emission at the Outer Edge of Protoplanetary Disks (2008, background): “The velocity fields of these disks all appear to be well described by Keplerian rotation (Isella et al. 2007; Qi et al. 2004; Dutrey et al. 1998; Piétu et al. 2007).”
• STRUCTURE AND EVOLUTION OF PRE-MAIN-SEQUENCE CIRCUMSTELLAR DISKS (2009, background): “…DN Tau, DM Tau, LkCa15, UZ Tau E, GM Aur, GSS39, SR24, TW Hya and MWC 275 both inclinations and position angles are in agreement with published values within 2σ (Jensen et al. 1996; Dutrey et al. 1997; Simon et al. 2000; Qi et al. 2004; Piétu et al. 2006; Andrews et al. 2007; Isella et al. 2007).”
• The Disk Substructures at High Angular Resolution Project (DSHARP). II. Characteristics of Annular Substructures (2018, methodology): “…Hya substructure positions are measured using the same procedure described for the other sources, except the P.A. is fixed to 155◦ and the inclination to 7◦ because nearly face-on disk orientations are more reliably measured from gas observations than from continuum observations (Qi et al. 2004).”
• EMPIRICAL CONSTRAINTS ON TURBULENCE IN PROTOPLANETARY ACCRETION DISKS (2010, methodology): “…stars, although they have also been demonstrated to be successful at reproducing spatially resolved dust continuum emission at millimeter wavelengths (see, e.g., Calvet et al. 2002; Hughes et al. 2007, 2009a) as well as spatially-resolved molecular line emission (see, e.g., Qi et al. 2004, 2006).”
• A Keplerian disk around a Class 0 source: ALMA observations of VLA1623A (2013, background): “…observed using molecular lines in the Class II stage of star formation (Mannings & Sargent 1997; Guilloteau & Dutrey 1998; Guilloteau et al. 1999; Qi et al. 2004; Hughes et al. 2009; Rodriguez et al. 2010), while continuum disk-like structures, the so-called pseudo-disks, are reported in Class 0…”