Star cluster formation in Orion A

Lim, Wanggi; Nakamura, Fúmitaka; Wu, Benjamin; Bisbas, Thomas G.; Tan, Jonathan C.; Chambers, E. T.; Bally, John; Kong, Shuo; McGehee, P.; Lis, D. C.; Ossenkopf-Okada, Volker; Sánchez-Monge, Á.

doi:10.1093/pasj/psaa035

Cited by 14 publications

(9 citation statements)

References 57 publications

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“…Several recent papers have argued for a cloud-cloud collision scenario for the formation of the ONC (Fukui et al 2018;Lim et al 2021), L1641-N (Nakamura et al 2012), NGC 2023 (Yamada et al 2020), NGC 2024(Enokiya et al 2021), and NGC 2068/2071(Fujita et al 2021 in the Orion complex. The cloud-cloud collision argument is made based on the analysis of the radial velocity of the CO gas, in particular a jump in the velocities at particular star formation rich regions, such as the head of the Orion A cloud.…”

Section: Implications For the Cloud-cloud Collision Scenario For The ...mentioning

confidence: 99%

3D dynamics of the Orion cloud complex

Großschedl

Alves

Meingast

et al. 2021

A&A

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We present the first study of the three-dimensional (3D) dynamics of the gas in the entire southern Orion cloud complex. We used the parallaxes and proper motions of young stellar objects (YSOs) from Gaia DR2 as a proxy for gas distance and proper motion, and the gas radial velocities from archival CO data, to compute the space motions of the different star-forming clouds in the complex, including subregions in Orion A, Orion B, and two outlying cometary clouds. From the analysis of the clouds’ orbits in space and time, we find that they were closest about 6 Myr ago and are moving radially away from roughly the same region in space. This coherent 100-pc scale radial motion supports a scenario where the entire complex is reacting to a major feedback event, which we name the Orion-BB (big blast) event. This event, which we tentatively associate with the recently discovered Orion X stellar population, shaped the distribution and kinematics of the gas we observe today, although it is unlikely to have been the sole major feedback event in the region. We argue that the dynamics of most of the YSOs carry the memory of the feedback-driven star formation history in Orion and that the majority of the young stars in this complex are a product of large-scale triggering, which can raise the star formation rate by at least an order of magnitude, as for the head of Orion A (the Integral Shape Filament). Our results imply that a feedback, compression, and triggering process lies at the genesis of the Orion Nebula Cluster and NGC 2023/2024 in Orion B, thus confirming broadly the classical feedback-driven scenario proposed in Elmegreen & Lada (1977, ApJ, 214, 725). The space motions of the well-known young compact clusters, σ Orionis and NGC 1977, are consistent with this scenario. A momentum estimate suggests that the energy of a few to several supernovae is needed to power the coherent 3D gas motion we measure in this paper.

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Section: Implications For the Cloud-cloud Collision Scenario For The ...mentioning

confidence: 99%

3D dynamics of the Orion cloud complex

Großschedl

Alves

Meingast

et al. 2021

A&A

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“…YSOs are stars at the very early stage of stellar evolution and are usually close to where they were born, such that they inhibit the velocity of gas from which they originate and their locations may indicate the shape of molecular clouds. Großschedl et al (2021); Lim et al (2021) compared the velocities of YSOs against the velocity of the ambient molecular gas, and found a good agreement. This technique has already been used in previous studies to study e.g.…”

Section: Introductionmentioning

confidence: 85%

Kinematics of the molecular interstellar medium probed by Gaia: steep velocity dispersion-size relation, isotropic turbulence, and location-dependent energy dissipation

Zhou,

Li,

Chen

2021

Preprint

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The morphology and kinematics of the molecular interstellar medium are controlled by processes such as turbulence, gravity, stellar feedback, and Galactic shear. Using a sample of 15149 young stellar objects (YSOs) with Gaia Data Release 2 (DR2) astrometric measurements, we study morphology and kinematic structure of their associated molecular gas. We identify 150 YSO associations with distance 𝑑 3 kpc. The YSO associations are oriented parallel to the disk midplane, with a median angle of 30 • , and they have a median aspect ratio of 1.97. Along the Galactic longitude direction, the velocity dispersion is related to the separation by 𝜎 𝑣 𝑙 = 0.58 (𝑟 𝑙 /pc) 0.66±0.05 (km s −1 ), along the Galactic latitude direction, 𝜎 𝑣 𝑏 = 0.54 (𝑟 𝑏 /pc) 0.64±0.04 (km s −1 ), and overall 𝜎 𝑣 ,2D = 0.74 (𝑟/pc) 0.67±0.05 (km s −1 ). The slope is on the stepper side, yet consistent with previous measurements. The energy dissipation rate of turbulence 𝜖 = 𝜎 3 𝑣,3D /𝐿 decreases with the Galactocentric distance 𝑟 gal by 𝜖 = 1.77 × 10 −4 𝑒 −0.45 (𝑟 gal /kpc) (erg g −1 s −1 ) for clouds with 40 pc < 𝑟 < 130 pc, which corresponds to a gradient of 0.2 dex kpc −1 . This decrease can be explained if turbulence is driven by cloud collisions, as the clouds located in the inner Galaxy have higher chances to accrete smaller clouds. Although the density structures of the complexes are anisotropic, the turbulence is consistent with being isotropic. Thus, the clouds are long-lived, stationary structures shaped by the Galactic motion where turbulence is maintained by a continuous injection.

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“…The shock wave of HB 3 may have plowed through YSOs and located them at the southern shell of the SNR. Recent studies show that the relatively older YSO populations have a higher spatial difference to the birthplace (Elmegreen 2018) or the higher kinematic difference from the dense molecular clouds (Lim et al 2021). The HB 3 regions also have been assumed to experience the repeated powerful feedback from the massive progenitor of HB 3 (e.g., Zhou et al 2016).…”

Section: Objectsmentioning

confidence: 99%

Shocked Molecular Hydrogen and Broad CO lines from the Interacting Supernova Remnant HB 3

Rho,

Jarrett,

Tram

et al. 2021

Preprint

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We present the detections of shocked molecular hydrogen (H 2 ) gas in near-and mid-infrared and broad CO in millimeter from the mixed-morphology supernova remnant (SNR) HB 3 (G132.7+1.3) using Palomar WIRC, the Spitzer GLIMPSE360 and WISE surveys, and HHSMT. Our near-infrared narrow-band filter H 2 2.12 µm images of HB 3 show that both Spitzer IRAC and WISE 4.6µm emission originates from shocked H 2 gas. The morphology of H 2 exhibits thin filamentary structures and a large scale of interaction sites between the HB 3 and nearby molecular clouds. Half of HB 3, the southern and eastern shell of the SNR, emits H 2 in a shape of a "butterfly" or "W", indicating the interaction sites between the SNR and dense molecular clouds. Interestingly, the H 2 emitting region in the south-east is also co-spatial to the interacting area between HB 3 and the H II regions of the W3 complex, where we identified star-forming activity.We further explore the interaction between HB 3 and dense molecular clouds with detections of broad CO(3-2) and CO(2-1) molecular lines from the southern and southeastern shell along the H 2 emitting region. The widths of the broad lines are 8-20 km s −1 ; the detection of such broad lines is unambiguous, dynamic evidence of the interactions between the SNR and clouds. The CO broad lines are from two branches of the bright, southern H 2 shell. We apply the Paris-Durham shock model to the CO line profiles, which infer the shock velocities of 20 -40 km s −1 , relatively low densities of 10 3−4 cm −3 and strong (>200 µG) magnetic fields.

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Star cluster formation in Orion A

Cited by 14 publications

References 57 publications

3D dynamics of the Orion cloud complex

3D dynamics of the Orion cloud complex

Kinematics of the molecular interstellar medium probed by Gaia: steep velocity dispersion-size relation, isotropic turbulence, and location-dependent energy dissipation

Shocked Molecular Hydrogen and Broad CO lines from the Interacting Supernova Remnant HB 3

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