Nested dust shells around the Wolf–Rayet binary WR 140 observed with JWST

Lau, Ryan M.; Hankins, Matthew J.; Han, Yinuo; Argyriou, Ioannis; Corcoran, M. F.; Eldridge, J. J.; Endo, Izumi; Fox, O.; Marín, Macarena García; Gull, Theodore R.; Jones, O. C.; Hamaguchi, Kenji; Lamberts, Astrid; Law, David R.; Madura, Thomas; Марченко, С. В.; Matsuhara, Hideo; Moffat, Anthony F. J.; Morris, Mark; Morris, P.; Onaka, Takashi; Ressler, Michael E.; Richardson, Noel D.; Russell, Christopher M. P.; Sánchez-Bermúdez, J.; Smith, Nathan; Soulain, A.; Stevens, I. R.; Tuthill, P. G.; Weigelt, G.; Williams, P. M.; Yamaguchi, Ryodai

doi:10.1038/s41550-022-01812-x

Cited by 37 publications

(31 citation statements)

References 42 publications

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“…The dearth of dust is in line with dust production models, which typically require several tens of Myr before the supernovae of the heaviest stars produce the metals necessary for dust. Wolf-Rayet stars are an alternative dust production pathway, where the orbital dynamics of two binary stars creates a region, where stellar winds are able to produce dust (Lau et al 2022 ). We can place a relatively weak constraint on the dust production from these types of systems down to < 1.5 × 10 −3 M star −1 in line with models by Lau et al ( 2021 ).…”

Section: Lack Of Dust In the Cosmic Dawn?supporting

confidence: 73%

Deep ALMA redshift search of a z ∼ 12 GLASS-JWST galaxy candidate

Bakx

Zavala

Mitsuhashi

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The James Webb Space Telescope (JWST) has discovered a surprising abundance of bright galaxy candidates in the very early Universe (≤500 Myrs after the Big Bang), calling into question current galaxy formation models. Spectroscopy is needed to confirm the primeval nature of these candidates, as well as to understand how the first galaxies form stars and grow. Here we present deep spectroscopic and continuum ALMA observations towards GHZ2/GLASS-z12, one of the brightest and most robust candidates at z > 10 identified in the GLASS-JWST Early Release Science Program. We detect a 5.8σ line, offset 0.″5 from the JWST position of GHZ2/GLASS-z12 that, associating it with the [O iii] 88 $\mu {\rm m}$ transition, implies a spectroscopic redshift of z = 12.117 ± 0.001. We verify the detection using extensive statistical tests. The oxygen line luminosity places GHZ2/GLASS-z12 above the [O iii]-SFR relation for metal-poor galaxies, implying an enhancement of [O iii] emission in this system while the JWST-observed emission is likely a lower-metallicity region. The lack of dust emission seen by these observations is consistent with the blue UV slope observed by JWST, which suggest little dust attenuation in galaxies at this early epoch. Further observations will unambiguously confirm the redshift and shed light on the origins of the wide and offset line and physical properties of this early galaxy. This work illustrates the synergy between JWST and ALMA and paves the way for future spectroscopic surveys of z > 10 galaxy candidates.

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Section: Lack Of Dust In the Cosmic Dawn?supporting

confidence: 73%

Deep ALMA redshift search of a z ∼ 12 GLASS-JWST galaxy candidate

Bakx

Zavala

Mitsuhashi

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…WR 140 is one of the archetypal CWBs, exhibiting time-dependent Xray (Pollock et al 2021;Miyamoto et al 2022) and radio (Dougherty et al 2005) emission with a 7.9 year period. The system is highly eccentric (𝑒 = 0.8993; Thomas et al 2021), and produces large quantities of dust near periastron (Williams et al 2009;Lau et al 2022). Dougherty et al (2005) spatially resolved the synchrotron emission from the shocked wind with radio interferometry, and this was further interpreted by Pittard & Dougherty (2006) in the context of an analytic model of particle acceleration and radiation.…”

Section: Wr 140 As a Case Study For Ic Coolingmentioning

confidence: 96%

“…3D hydrodynamical simulations of the WR 140 (Eatson et al 2022b) and WR 104 (Soulain et al 2023) systems including models of dust-grain growth have been presented to compare with existing observations and in anticipation of new results with JWST. Dust shells in the WR 140 system were recently observed using ground-based near-IR imaging (Han et al 2022) and JWST mid-IR images (Lau et al 2022). The extreme CWB Apep was also observed at high angular resolution by Han et al (2020), spatially resolving the dust plume.…”

Section: Introductionmentioning

confidence: 96%

Inverse Compton cooling of thermal plasma in colliding-wind binaries

Mackey¹,

Jones²,

Brose³

et al. 2023

Preprint

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The inverse-Compton effect (IC) is a widely recognized cooling mechanism for both relativistic and thermal electrons in various astrophysical environments, including the intergalactic medium and X-ray emitting plasmas. Its effect on thermal electrons is however frequently overlooked in theoretical and numerical models of colliding-wind binaries (CWB). In this article, we provide a comprehensive investigation of the impact of IC cooling in CWBs, presenting general results for when the photon fields of the stars dominate the cooling of the thermal plasma and when shocks at the stagnation point are expected to be radiative. Our analysis shows that IC cooling is the primary cooling process for the shocked-wind layer over a significant portion of the relevant parameter space, particularly in eccentric systems with large wind-momentum ratios, e.g., those containing a Wolf-Rayet and O-type star. Using the binary system WR 140 as a case study, we demonstrate that IC cooling leads to a strongly radiative shocked wind near periastron, which may otherwise remain adiabatic if only collisional cooling was considered. Our results are further supported by 2D and 3D simulations, which illustrate the impact of including or neglecting IC cooling. Specifically, 3D magnetohydrodynamic simulations of WR 140 show a significant decrease in hard-X-ray emission around periastron, in agreement with observations but in contrast to equivalent simulations that omit IC cooling. A novel method is proposed for constraining mass-loss rates of both stars in eccentric binaries where the wind-collision zone switches from adiabatic to radiative approaching periastron. This study highlights the importance of including the IC process for thermal electrons in theoretical and numerical models of colliding-wind binaries.

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“…If seeds are present in the first place, grain growth should be efficient at high densities log n e = 4-5 and a cool gas temperature at a few thousand K, even under strong external UV irradiation. For example, dust grains are observed to rapidly form in colliding wind shells of the Wolf-Rayet binary system WR140 (Han et al 2022;Lau et al 2022).…”

Section: Element Abundancesmentioning

confidence: 99%

The Lyman-continuum-leaking super star cluster in the Sunburst Arc and its surrounding nebula

Pascale¹,

Dai²,

McKee³

et al. 2023

Preprint

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Strong lensing offers a precious opportunity for studying the formation and early evolution of super star clusters that are rare in our cosmic backyard. The Sunburst Arc, a lensed Cosmic Noon galaxy, hosts a young super star cluster with escaping Lyman continuum radiation. Analyzing archival HST images and emission line data from VLT/MUSE and X-shooter, we construct a physical model for the cluster and its surrounding photoionized nebula. We confirm that the cluster is ∼ 3-4 Myr old, is extremely massive M ∼ 10 7 M and yet has a central component as compact as several parsecs, and we find a metallicity Z = (0.26±0.03) Z . The cluster is surrounded by 10 5 M of dense clouds that have been pressurized to P ∼ 10 9 K cm −3 by perhaps stellar radiation at within ten parsecs. These should have large neutral columns N HI > 10 22.5 cm −2 to survive rapid ejection by radiation pressure. The clouds are likely dusty as they show gas-phase depletion of silicon, and may be conducive to secondary star formation if N HI > 10 24 cm −2 or if they sink further toward the cluster center. Detecting strong N III]λλ1750,1752, we infer heavy nitrogen enrichment log(N/O) = −0.23 +0.08 −0.11 . This requires efficiently retaining 500 M of nitrogen in the high-pressure clouds from massive stars heavier than 60 M up to 4 Myr. We suggest a physical origin of the high-pressure clouds from partial or complete condensation of slow massive star ejecta, which may have important implication for the puzzle of multiple stellar populations in globular clusters.

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Nested dust shells around the Wolf–Rayet binary WR 140 observed with JWST

Abstract: x the JWST/MIRI observations that reveal the spectral and spatial signatures of dust around WR 140: over 17 nested dust shells from the past ≳130 yr of episodic dust production and the mid-IR spectroscopic signatures from the direct emission of WC dust.

Cited by 37 publications

References 42 publications

Deep ALMA redshift search of a z ∼ 12 GLASS-JWST galaxy candidate

Deep ALMA redshift search of a z ∼ 12 GLASS-JWST galaxy candidate

Inverse Compton cooling of thermal plasma in colliding-wind binaries

The Lyman-continuum-leaking super star cluster in the Sunburst Arc and its surrounding nebula

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