Observations of warm molecular gas and kinematics in the disc around HD 100546

Abstract

Context. The disc around the Herbig Ae/Be star HD 100546 is one of the most extensively studied discs in the southern sky. Although there is a wealth of information about its dust content and composition, not much is known about its gas and large-scale kinematics. Many recent results have stressed the importance of studying both the gas and dust in discs. 12 CO is an excellent gas tracer in the submillimetre, and the intensity ratio between lines originating from low and high rotational levels probes the gas temperature. Emerging submillimetre facilities in the Southern hemisphere allow us to characterise the gas and dust content in objects like HD 100546 better. Aims. Our aim is to establish whether the disc is gas-rich and to study the disc temperature and kinematics. Methods. We detected and studied the molecular gas in the disc at spatial resolution from 7. 7 to 18. 9 using the Atacama Pathfinder Experiment telescope . We observed the lines 12 CO J = 7−6, J = 6−5, J = 3−2, 13 CO J = 3−2 and [C I] 3 P 2 − 3 P 1 , as diagnostics of disc temperature, size, chemistry, and kinematics. We use parametric disc models that reproduce the low-J 12 CO emission from Herbig Ae stars and we vary the basic disc parameters -temperature, mass, and size. With the help of a molecular excitation and radiative transfer code we fit the observed spectral line profiles. Results. Our observations are consistent with more than 10 −3 M of molecular gas in a disc of ≈400 AU radius in Keplerian rotation around a 2.5 M star, seen at an inclination of 50 • . The detected 12 CO lines are dominated by gas at 30−70 K. Not detecting the [C I] line indicates excess ultraviolet emission above that of a B9 type model stellar atmosphere. Asymmetry in the 12 CO line emission suggests that one side of the outer disc is colder by 10−20 K than the other. A plausible scenario is a warped geometry in the inner disc casting a partial shaddow on the outer disc. We exclude pointing offsets, foreground cloud absorption, and asymmetry in the disc extent as possible causes of the observed line asymmetry. Conclusions. Efficient heating of the outer disc by the star HD 100546 ensures that low-and high-J 12 CO lines are dominated by the outermost disc regions, indicating a 400 AU radius. The 12 CO J = 6−5 line arises from a disc layer higher than disc midplane, and warmer by 15−20 K than the layer emitting the J = 3−2 line. The existing models of discs around Herbig Ae stars, asuming a B9.5 type model stellar atmosphere, overproduce the [CI] 3 P 2 − 3 P 1 line intensity from HD 100546 by an order of magnitude.

First results of theHerschelkey program “Dust, Ice and Gas In Time” (DIGIT): Dust and gas spectroscopy of HD 100546

“…The latter was fitted with a column density of at least 2.3×10 15 cm −2 (for discussion, see Brittain et al 2009). The submillimeter data give a typical CO column density of 10 18 cm −2 (Panić et al 2010). From Fig.…”

“…Observations of optical [O i] and Balmer line emission, on the other hand, demonstrate that the inner disk is not completely devoid of gas (Acke & van den Ancker 2006). At submillimetre wavelengths, Panić et al (2010) have A&A 518, L129 (2010) detected pure rotational lines of CO up to J = 7−6 probing a warm (60-70 K) layer in the outer disk (∼100 AU). Information on the intermediate temperatures is still lacking.…”

Planet or brown dwarf? Inferring the companion mass in HD 100546 from the wall shape using mid-infrared interferometry

“…A better definition would involve whether the formation process of the companion occured in a disk or like a single star. The current gas mass of the disk is uncertain due to lack of resolved millimeter observations, but is estimated to be in the range 0.0005 to 0.01 M (Panić et al 2010;Thi et al 2011) and therefore much lighter than the planet, making it unlikely that the planet recently formed out of the disk.…”

DIGIT survey of far-infrared lines from protoplanetary discs

“…5. Lines with J up ≤ 7 are convolved to the beam of the APEX telescope, which has been used to detect these lines towards Herbig discs (e.g., Panić et al 2010). Higher J up lines are convolved to the beam of the PACS instrument.…”