Chemical complexity in high-mass star formation

Abstract

Aims. In order to understand the observed molecular diversity in high-mass star-forming regions, we have to determine the underlying physical and chemical structure of those regions at high angular resolution and over a range of evolutionary stages. Methods. We present a detailed observational and modeling study of the hot core VLA 3 in the high-mass star-forming region AFGL 2591, which is a target region of the NOrthern Extended Millimeter Array (NOEMA) large program CORE. Using NOEMA observations at 1.37 mm with an angular resolution of ~0″. 42 (1400 au at 3.33 kpc), we derived the physical and chemical structure of the source. We modeled the observed molecular abundances with the chemical evolution code MUSCLE (MUlti Stage ChemicaL codE). Results. With the kinetic temperature tracers CH3CN and H2CO we observe a temperature distribution with a power-law index of q = 0.41 ± 0.08. Using the visibilities of the continuum emission we derive a density structure with a power-law index of p = 1.7 ± 0.1. The hot core spectra reveal high molecular abundances and a rich diversity in complex molecules. The majority of the molecules have an asymmetric spatial distribution around the forming protostar(s), which indicates a complex physical structure on scales <1400 au. Using MUSCLE, we are able to explain the observed molecular abundance of 10 out of 14 modeled species at an estimated hot core chemical age of ~21 100 yr. In contrast to the observational analysis, our chemical modeling predicts a lower density power-law index of p < 1.4. Reasons for this discrepancy are discussed. Conclusions. Combining high spatial resolution observations with detailed chemical modeling allows us to derive a concise picture of the physical and chemical structure of the famous AFGL 2591 hot core. The next steps are to conduct a similar analysis for the whole CORE sample, and then use this analysis to constrain the chemical diversity in high-mass star formation to a much greater depth.

From clump to disc scales in W3 IRS4

“…While not as chemically rich as some other sources in the CORE sample (for example AFGL2591 or W3 OH/H 2 O, see Beuther et al 2018;Gieser et al 2019;Ahmadi et al 2018), the W3 IRS4 region does show a reasonable degree of chemical complexity, particularly at the position of IRS4 itself (see Fig. 14).…”

On the pumping of the CS(υ = 0) masers in W51 e2e

“…Another factor may be the geometry of the masing region which can affect the beaming and therefore the brightness of the masers. It was found that beaming which is stronger than that given by Elitzur (1992) but similar to that found by Spaans & van Langevelde (1992) is needed to explain the observed brightness temperatures of the masers. However it should not be as strong as that used by Sobolev et al (1997).…”

“…When a population inversion occurs, beaming becomes important in which case Eq. 3 becomes (Elitzur 1992) with Ω i j /4π the fractional beam solid angle. According to Elitzur (1992), Ω i j /4π = (2τ i j ) −1 .…”

“…3 becomes (Elitzur 1992) with Ω i j /4π the fractional beam solid angle. According to Elitzur (1992), Ω i j /4π = (2τ i j ) −1 . This dependence suggests that beaming only starts when τ i j = 0.5.…”

“…On the other hand, Spaans & van Langevelde (1992) argued that Ω i j /4π ≈ τ −2 i j . We combined these two and assumed the beaming factor to be of the form Ω i j /4π = (2τ i j + 1) −η to allow for beaming to start as soon as a population inversion occurs as well as to consider stronger beaming than that of Elitzur (1992).…”