A Molecular Inventory of the L1489 IRS Protoplanetary Disk Michiel R. Hogerheijde Christian Brinch Leiden Observatory Jes K. Joergensen CfA

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA Origin of Protoplanetary Disks It’s the angular momentum, stupid Initial distribution of angular momentum –E.g., Goodman et al. 1998; Ohashi et al. 1997; Belloche et al Redistribution during collapse Formation of a viscous disk –Mass, size, evolution with time, accretion shock –E.g., Stahler 1994; Velusamy et al. 2002

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA L1489 IRS: A Transitional Object? Compact dust continuum –2000 AU radius –Density: radial power law with slope 1.8–2.1 –Mass 0.01–0.02 M  –Hogerheijde & Sandell 2000; Joergensen et al Neighboring prestellar core SCUBA 850 and 450 µm observations from Hogerheijde & Sandell (2000)

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA L1489 IRS: A Transitional Object? Single-dish HCO + lines –infall Interferometer HCO + image –Rotation Hogerheijde (2001) CO 4.5 µm absorption lines –Inward motions continue to within 0.1 AU from star Boogert et al. (2002) Hogerheijde (2001)

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA L1489 IRS: A Transitional Object? Single-dish HCO + lines –infall Interferometer HCO + image –Rotation Hogerheijde (2001) CO 4.5 µm absorption lines –Inward motions continue to within 0.1 AU from star Boogert et al. (2002) Hogerheijde (2001) HCO + 1.1mm BIMA 2000

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA L1489 IRS: A Transitional Object? NICMOS scattered light suggests flared disk –Padgett et al. (1998) Simple model –Flared disk –10% infall, 90% rotation –Hogerheijde (2001) Transitional, short-lived (2x10 4 yr) stage between embedded and T Tauri phase? NICMOS image from Padgett et al. (1998)

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA Molecular Line Survey Single-dish molecular line measurements –JCMT, IRAM 30m, and Onsala 20m: 14”–38” = 2000–5500 AU –C 17 O 1–0, 2–1, 3–2 –C 18 O 1–0, 2–1, 3–2 –CS 2–1, 5–4, 7–6 –C 34 S 2–1, 5–4 –HCO + 1–0, 3–2, 4–3 –H 13 CO + 1–0, 3–2 –CN 1–0, 3–2 –HCN 1–0, 4–3 –H 13 CN 1–0 –HNC 4–3 Aims –More realistic model –Chemical inventory

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA Modeling Approach Physical model: density –Flattened Plummer sphere Consistent with SCUBA data p=1.8 (Joergensen et al. 2002) Brinch, Hogerheijde, & Joergensen (in prep) (Joergensen et al. 2002)

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA Modeling Approach Physical model: density –Flattened Plummer sphere Consistent with SCUBA data p=1.8 (Joergensen et al. 2002) f>0 Brinch, Hogerheijde, & Joergensen (in prep)

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA Modeling Approach Velocity field –Rotation V   √M * r -0.5 –Infall V r  √M * r -0.5 Parameterize V-field by –|V|  √M * r -0.5 –tg(  )=V r /V   Brinch, Hogerheijde, & Joergensen (in prep) V VV VrVr

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA Modeling Approach  2 minimization of synthetic single-dish spectra –Gridded physical model + (constant) abundances –Molecular excitation using Monte Carlo approach –Synthetic spectra, convolved to appropriate resolution 4+n free parameters –Flattening parameter f –Inclination i –Stellar mass M * –Velocity field direction angle  –Molecular Abundances X i Brinch, Hogerheijde, & Joergensen (in prep)

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA Results Brinch, Hogerheijde, & Joergensen (in prep)

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA Results Brinch, Hogerheijde, & Joergensen (in prep)

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA Results Brinch, Hogerheijde, & Joergensen (in prep)

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA Results Preliminary values –Stellar mass 1.1 M  –Flattening parameter f=3.0 Equivalent with h/R=0.35 –Inclination 70˚ –Velocity field angle  =18˚ Inspiral time approximately 10 5 yr Significant fraction of embedded life time Brinch, Hogerheijde, & Joergensen (in prep)

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA Results Abundances –C 18 O 4x10 -7 (-> 12 CO 2x10 -4 no depletion) –CS 8x10 -9 –SO 8x10 -9 –H 2 CO 1x10 -9 –HCO + 4x10 -8 –HCN 4x10 -9 –HNC 2x10 -9 –CN 2x10 -9 Dark cloud values; little depletion; HCO + increased? Brinch, Hogerheijde, & Joergensen (in prep)

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA HCO + 1–0 Interferometry ObservationsModel Prediction Brinch, Hogerheijde, & Joergensen (in prep) Surrounding cloud material

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA Enhanced-SMA Predictions SMA CSO JCMT

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA Enhanced-SMA Predictions Brinch, Hogerheijde, & Joergensen (in prep) HCO + 4–3 at 0.3” (40 AU)

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA A break in the V-field at 300 AU Brinch, Hogerheijde, & Joergensen (in prep) HCO + 4–3 at 0.3” (40 AU)

Submillimeter Astronomy in the Era of the SMA June 13– Cambridge MA Conclusion L1489 IRS –Disklike rotating and infalling structure –Lifetime 10 5 yr, significant fraction of embedded phase –Chemical abundances No evidence for depletion HCO + enhanced Further high-resolution observations with, e.g., enhanced-SMA –Breaks in the velocity field on scales of T Tauri disks –Changes in the chemistry on scales of T Tauri disks