Euclid: 对 ERO/普莱斯德域首次统计性调查尘埃覆盖且质量巨大的天体
星系天体物理
2026-02-25 v1
摘要
对 z>3 星际形成历史的理解依赖于 rest 框架的 UV 观测，但此选择会遗漏最尘埃覆盖且质量最大的源体，导致早期时期的统计不完整。红外设施如 Spitzer 和詹姆斯·韦伯太空望远镜揭示了在 z=3-6 处具有极端红色颜色的隐藏人群，称为 HIEROs（HST-to-IRAC 极端红色天体），通过标准 H_{\mathrm{E}}-\mathrm{ch2}>2.25 进行识别。最近，Euclid 早期释放观测 (ERO) 使得通过比较 Euclid 数据与辅助 Spitzer/IRAC 成像进一步研究此类天体成为可能。在本文中，我们使用 VIS 和 NISP 光度学，结合四个 Spitzer 通道和地面 MegaCam 波段 (u, g, r, \mathrm{H}\alpha, i, z)，调查普莱斯德域 232 平方弧分^2 的区域。应用颜色切割后，我们得到 121 个 HIEROs；通过对多波段切片进行视觉检查去除星际云、棕矮星以及不可靠案例后，我们最终获得 42 个可靠的 HIEROs。使用 SED 拟合代码 Bagpipes 估计光度红移和物理属性。基于得到的 z_{\mathrm{phot}} 和 M_* 数据，我们计算了 3.5<z<5.5 区间的星系恒星质量函数。即便在排除可能的 AGN 宿主或星系质量可能被高估的系统后，高质量端仍与之前的测定相当，表明真实丰度可能更高。这些结果凸显了进一步研究此类遮蔽人群以评估其在宇宙星际形成率密度中的作用及其与星系形成模型的一致性的重要性，展示了 Euclid 在跨早期时代理解尘埃隐藏星际形成方面的能力。
引用
@article{arxiv.2512.01489,
title = {Euclid: The first statistical census of dusty and massive objects in the ERO/Perseus field},
author = {G. Girardi and A. Grazian and G. Rodighiero and L. Bisigello and G. Gandolfi and E. Bañados and S. Belladitta and J. R. Weaver and S. Eales and C. C. Lovell and K. I. Caputi and A. Enia and A. Bianchetti and E. Dalla Bontà and T. Saifollahi and A. Vietri and N. Aghanim and B. Altieri and S. Andreon and N. Auricchio and H. Aussel and C. Baccigalupi and M. Baldi and A. Balestra and S. Bardelli and P. Battaglia and A. Biviano and E. Branchini and M. Brescia and J. Brinchmann and S. Camera and G. Cañas-Herrera and V. Capobianco and C. Carbone and J. Carretero and S. Casas and M. Castellano and G. Castignani and S. Cavuoti and K. C. Chambers and A. Cimatti and C. Colodro-Conde and G. Congedo and C. J. Conselice and L. Conversi and Y. Copin and F. Courbin and H. M. Courtois and M. Cropper and A. Da Silva and H. Degaudenzi and G. De Lucia and A. M. Di Giorgio and H. Dole and M. Douspis and F. Dubath and C. A. J. Duncan and X. Dupac and S. Dusini and S. Escoffier and M. Farina and R. Farinelli and F. Faustini and S. Ferriol and S. Fotopoulou and M. Frailis and E. Franceschi and M. Fumana and S. Galeotta and K. George and B. Gillis and C. Giocoli and J. Gracia-Carpio and F. Grupp and S. V. H. Haugan and J. Hoar and W. Holmes and I. M. Hook and F. Hormuth and A. Hornstrup and P. Hudelot and K. Jahnke and M. Jhabvala and E. Keihänen and S. Kermiche and A. Kiessling and B. Kubik and M. Kümmel and M. Kunz and H. Kurki-Suonio and A. M. C. Le Brun and D. Le Mignant and P. Liebing and S. Ligori and P. B. Lilje and V. Lindholm and I. Lloro and G. Mainetti and D. Maino and E. Maiorano and O. Mansutti and S. Marcin and O. Marggraf and M. Martinelli and N. Martinet and F. Marulli and R. Massey and S. Maurogordato and E. Medinaceli and S. Mei and Y. Mellier and M. Meneghetti and E. Merlin and G. Meylan and A. Mora and M. Moresco and L. Moscardini and R. Nakajima and C. Neissner and R. C. Nichol and S. -M. Niemi and C. Padilla and S. Paltani and F. Pasian and K. Pedersen and W. J. Percival and V. Pettorino and G. Polenta and M. Poncet and L. A. Popa and L. Pozzetti and F. Raison and R. Rebolo and A. Renzi and J. Rhodes and G. Riccio and E. Romelli and M. Roncarelli and E. Rossetti and B. Rusholme and R. Saglia and Z. Sakr and D. Sapone and B. Sartoris and J. A. Schewtschenko and P. Schneider and T. Schrabback and A. Secroun and G. Seidel and M. Seiffert and S. Serrano and P. Simon and C. Sirignano and G. Sirri and L. Stanco and J. Steinwagner and P. Tallada-Crespí and D. Tavagnacco and A. N. Taylor and I. Tereno and R. Toledo-Moreo and F. Torradeflot and I. Tutusaus and L. Valenziano and J. Valiviita and T. Vassallo and G. Verdoes Kleijn and A. Veropalumbo and Y. Wang and J. Weller and G. Zamorani and F. M. Zerbi and E. Zucca and M. Bolzonella and C. Burigana and L. Gabarra and J. Martín-Fleitas and V. Scottez},
journal= {arXiv preprint arXiv:2512.01489},
year = {2026}
}
备注
23 pages, 8 figures. Accepted for publication in A\&A