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The average dust attenuation curve at z ∼ 1.3 based on HST grism surveys

Battisti, A. J. and Bagley, M. B. and Baronchelli, I. and Dai, Y. S. and Henry, A. L. and Malkan, M. A. and Alavi, A. and Calzetti, D. and Colbert, J. and McCarthy, P. J. and Mehta, V. and Rafelski, M. and Scarlata, C. and Shivaei, I. and Wisnioski, E. (2022) The average dust attenuation curve at z ∼ 1.3 based on HST grism surveys. Monthly Notices of the Royal Astronomical Society, 513 (3). pp. 4431-4450. ISSN 0035-8711. doi:10.1093/mnras/stac1052.

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We present the first characterization of the average dust attenuation curve at z ∼ 1.3 by combining rest-frame ultraviolet through near-IR photometry with Balmer decrement (H α/H β) constraints for ∼900 galaxies with 8 ≲ log (M⋆/M_⊙) < 10.2 at 0.75 < z < 1.5 in the HST WFC3 IR Spectroscopic Parallel and 3D-HST grism surveys. Using galaxies in SDSS, we establish that the (H α + [N ii])/[O iii] line ratio and stellar mass are good proxies for the Balmer decrement in low-spectral resolution grism data when only upper limits on H β are available and/or H α is blended with [N ii]. The slope of the z ∼ 1.3 attenuation curve (A(0.15 µm})/A(V) = 3.15) and its normalization (R_V = 3.26) lie in-between the values found for z = 0 and z ∼ 2 dust attenuation curves derived with similar methods. These provide supporting evidence that the average dust attenuation curve of star-forming galaxies evolves continuously with redshift. The z ∼ 1.3 curve has a mild 2175 Å feature (bump amplitude, E_b = 0.83; ∼25 per cent that of the MW extinction curve), which is comparable to several other studies at 0 < z ≲ 3, and suggests that the average strength of this feature may not evolve significantly with redshift. The methods we develop to constrain dust attenuation from HST grism data can be applied to future grism surveys with JWST, Euclid, and RST. These new facilities will detect millions of emission line galaxies and offer the opportunity to significantly improve our understanding of how and why dust attenuation curves evolve.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Battisti, A. J.0000-0003-4569-2285
Bagley, M. B.0000-0002-9921-9218
Baronchelli, I.0000-0003-0556-2929
Dai, Y. S.0000-0002-7928-416X
Henry, A. L.0000-0002-6586-4446
Malkan, M. A.0000-0001-6919-1237
Alavi, A.0000-0002-8630-6435
Calzetti, D.0000-0002-5189-8004
Colbert, J.0000-0001-6482-3020
Mehta, V.0000-0001-7166-6035
Rafelski, M.0000-0002-9946-4731
Scarlata, C.0000-0002-9136-8876
Shivaei, I.0000-0003-4702-7561
Wisnioski, E.0000-0003-1657-7878
Additional Information:© 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model ( Received: 07 January 2022. Revision received: 07 April 2022. Accepted: 08 April 2022. Published: 19 April 2022. The authors thank the anonymous referee, whose suggestions helped to clarify and improve the content of this work. Parts of this research were supported by the Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), through project number CE170100013. YSD acknowledges the support from National Key R&D Program of Chinavia grant no. 2017YFA0402704, the NSFC grants 11933003, and the China Manned Space Project with No. CMS-CSST-2021-A05. AJB thanks K. Grasha for comments that improved the paper. AJB thanks A. Faisst for helpful responses to inquiries pertaining to his paper. AJB is also thankful for attending ASTRO 3D writing retreats that provided a helpful environment to complete portions of this manuscript. We acknowledge the invaluable labor of the maintenance and clerical staff at our institutions, whose contributions make our scientific discoveries a reality. This research was conducted on Ngunnawal Indigenous land. DATA AVAILABILITY. All of the photometric and spectroscopic data used in this paper are publicly available through data releases from the WISP, 3D-HST, and SDSS survey teams as described in Section 2. Other data products can be made available upon reasonable request to the first author.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Australian Research CouncilCE170100013
National Key Research and Development Program of China2017YFA0402704
National Natural Science Foundation of China11933003
China Manned Space ProjectCMS-CSST-2021-A05
Subject Keywords:dust, extinction, ISM: evolution, galaxies: evolution, galaxies: ISM, galaxies: star formation
Issue or Number:3
Record Number:CaltechAUTHORS:20220802-743087000
Persistent URL:
Official Citation:A J Battisti, M B Bagley, I Baronchelli, Y S Dai, A L Henry, M A Malkan, A Alavi, D Calzetti, J Colbert, P J McCarthy, V Mehta, M Rafelski, C Scarlata, I Shivaei, E Wisnioski, The average dust attenuation curve at z ∼ 1.3 based on HST grism surveys, Monthly Notices of the Royal Astronomical Society, Volume 513, Issue 3, July 2022, Pages 4431–4450,
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:116019
Deposited By: George Porter
Deposited On:02 Aug 2022 21:02
Last Modified:02 Aug 2022 21:02

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