Nitrogen-enriched, Highly Pressurized Nebular Clouds Surrounding a Super Star Cluster at Cosmic Noon

IF 4.8 2区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Astrophysical Journal Pub Date : 2023-11-01 DOI:10.3847/1538-4357/acf75c
Massimo Pascale, Liang Dai, Christopher F. McKee, Benny T.-H. Tsang
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引用次数: 1

Abstract

Abstract 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 Hubble Space Telescope images and emission line data from Very Large Telescope/MUSE and X-shooter, we construct a physical model for the cluster and its surrounding photoionized nebula. We confirm that the cluster is ≲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 gas-phase metallicity Z = (0.22 ± 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 10 pc. These should have large neutral columns N HI > 10 22.8 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 farther toward the cluster center. Detecting strong [N iii ] λ λ 1750,1752, we infer heavy nitrogen enrichment log ( N / O ) = 0.21 0.11 + 0.10 . 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 an important implication for the puzzle of multiple stellar populations in globular clusters.
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富含氮的高压星云围绕着宇宙正午的超级星团
强透镜效应为研究在我们的宇宙后院中罕见的超级星团的形成和早期演化提供了宝贵的机会。太阳爆发弧,一个透镜状的宇宙正午星系,拥有一个逃离莱曼连续辐射的年轻超级星团。分析了哈勃太空望远镜的档案图像、甚大望远镜/MUSE和x -射手的发射线数据,我们构建了星团及其周围光电离星云的物理模型。我们确认该星系团的年龄小于4 Myr,质量非常大M - ~ 10.7 M⊙,但其中心成分的密度却只有几个秒差距,并且我们发现气相金属丰度Z =(0.22±0.03)Z⊙。星团周围环绕着质量约为10.5 M⊙的致密云,这些云可能是在10pc内被恒星辐射压缩到P ~ 10 9 K cm−3。这些应该有大的中性柱。10 22.8 cm−2才能在辐射压力下存活。这些云很可能是尘埃,因为它们显示了硅的气相耗尽,并且可能有利于次级恒星的形成。10 24 cm−2或者它们向星团中心进一步下沉。检测到强[N iii] λ λ 1750,1752,我们推断重氮富集对数(N / O) =−0.21−0.11 + 0.10。这需要在质量大于60 M⊙的大质量恒星的高压云中有效地保留约500 M⊙的氮,直至4myr。我们认为高压云的物理起源是缓慢的大质量恒星喷射物的部分或完全凝结,这可能对球状星团中多恒星群的谜题具有重要意义。
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来源期刊
Astrophysical Journal
Astrophysical Journal 地学天文-天文与天体物理
CiteScore
8.40
自引率
30.60%
发文量
2854
审稿时长
1 months
期刊介绍: The Astrophysical Journal is the foremost research journal in the world devoted to recent developments, discoveries, and theories in astronomy and astrophysics.
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