DISK KINEMATICS & FRAGMENTATION

DISK KINEMATICS & FRAGMENTATION IN HIGH-MASS STAR FORMATION

Zooming in on Star Formation Nafplio, Greece - June 13, 2019 + Team

Henrik Beuther Rolf Kuiper

Joe Mottram

LINKING OBSERVATIONS AND SIMULATIONS

June 13, 2019Aida Ahmadi zooming in on star formation - Nafplio, Greece

: IRAM NOEMA LARGE PROGRAM✦ Sample of 20 young high-luminosity regions: L > 104 L☉

✦ Dust continuum & line observations at 1.3 mm (220 GHz)

✦ NOEMA: Plateau de Bure + new antennae

✦ IRAM 30-m telescope data to cover the missing flux

A, B, & D configurations in decreasing baseline length

Highest resolution ~ 0.3” => 600 AU at 2 kpc

: MOTIVATION

✦ What are the fragmentation properties of high mass star forming

regions during the early evolutionary stages of cluster formation?

✦ How is the gas accumulated into the central cores and what are

the larger-scale gas accretion flow and infall properties?

✦ What are the chemical properties of distinct substructures within

high-mass star-forming regions?

✦ Can we identify genuine high-mass accretion disks, and if yes,

what are their properties?

Beuther et al. 2018

Ahmadi et al. 2018

Mottram et al. subm.

Gieser et al. subm.

: MOTIVATION

✦ What are the fragmentation properties of high mass star forming

regions during the early evolutionary stages of cluster formation?

✦ How is the gas accumulated into the central cores and what are

the larger-scale gas accretion flow and infall properties?

✦ What are the chemical properties of distinct substructures within

high-mass star-forming regions?

✦ Can we identify genuine high-mass accretion disks, and if yes, what are their properties?

Beuther et al. 2018

Ahmadi et al. 2018

Mottram et al. subm.

Gieser et al. subm.

: DUST CONTINUUMBeuther, Mottram, Ahmadi et al. 2018

data products: www.mpia.de/core/

CONTINUUM & VELOCITY STRUCTURE

✦ Velocity map of the region in CH3CN (123-113) shows clear gradient in the E-W direction

✦ Velocity gradient observed for each fragment consistent with molecular outflows

KINEMATICS OF FRAGMENTS

left fragment right fragment

Ahmadi et al. 2018

MODELLING WITH XCLASS

✦ XCLASS: solves the radiative transfer equation under LTE and generates synthetic spectra that can be compared to the real spectra

✦ Fitting CH3CN (12-11) k=4 to k =6 lines simultaneously along with their CH3

13CN isotopologues

T ~ 160 K

(EXTENDED CASA LINE ANALYSIS SOFTWARE SUITE)

W3(H2O) TEMPERATURE MAP

✦ Average temperature is warm: ~180 K

TOOMRE STABILITY

✦ For a differentially rotating disk, the shear force can provide added stability against collapse

✦ Quantified by Toomre (1964) via

✦ A thin disk becomes unstable against axisymmetric gravitational instabilities if Q < 1

epicyclic frequency of the disk = angular velocity for Keplerian rotation

surface density of the disk

sound speed

TOOMRE STABILITY

✦ Outer rotating structure is Toomre-unstable in parts

Ahmadi et al. 2018 UNCERTAINTIES

✦ Inclination angle

✦ Mass of disk & central object

✦ Further disk fragmentation possible

✦ Global collapse of a cloud of gas + dust with 200 M☉in 0.1 pc

RADIATION HYDRO SIMULATIONS

Oliva, Kuiper et al. (in prep.)

DETAILS✦ PLUTO code

✦ Initial mass density profile: 𝞺 ∝ r -1.5

✦ Spherical grid

✦ Outer edge of disk resolved down to 25 au

✦ Inner part resolved down to 0.75 au

✓ Jeans length resolved!

1.3 MM DUST CONTINUUM

distance: 2 kpc

0.07” (140 au)

distance: 2 kpc

0.4” (800 au)

KINEMATICS: CH3CN (124-114)

Moment 1 (peak velocity) maps at different inclinations

distance: 2 kpc

ALMA resolves the velocity structure well

distance: 2 kpc

In NOEMA observations, the emission is smeared out over a larger region

distance: 2 kpc

TOOMRE STABILITY: INCLINATIONS

‘true’ Toomre Q maps at different inclinations Q < 1 at the positions of fragments

Q < 1 at the positions of fragments Ahmadi, Kuiper & Beuther (submitted to A&A)

Although NOEMA wouldn’t resolve fragments at 2 kpc, the disk is asymmetrically unstable and fragmentation is predicted nonetheless

Method is robust in predicting disk fragmentation regardless of inclination uncertainties Ahmadi, Kuiper & Beuther (submitted to A&A)

KINEMATICS: PV MAPS

high-velocity components of Keplerian disk best seen at higher inclinations

KINEMATICS: PV MAPS

High-velocity components smeared out

: DUST CONTINUUMBeuther, Mottram, Ahmadi et al. 2018

: KINEMATICS

Ahmadi et al. in prep.

: TEMPERATURES

CONCLUSIONS

✦ High resolution observations needed to study early phase of high-mass star formation -> CORE survey

✦ Different modes of fragmentation

✦ Isolated cores vs. highly fragmented clumps

✦ Core fragmentation on large scales & disk fragmentation on small scales

✦ Rotating structures detected around most objects

✦ Benchmarked method to study disk stability

credit: Andre Rambaud

✦ Apply similar analyses to all other sources and study fragmentation and disk kinematics in a statistical way

OUTLOOK

DISK KINEMATICS & FRAGMENTATION

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