Maqola

What Is the Nature of Little Red Dots and what Is Not, MIRI SMILES Edition

Pablo G. Pérez‐GonzálezCentro de Astrobiología (CAB), CSIC-INTA, Ctra. de Ajalvir km 4, Torrejón de Ardoz, E-28850, Madrid, SpainGuillermo BarroDepartment of Physics, University of the Pacific, Stockton, CA 90340 USAG. H. RiekeSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USAJianwei LyuSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USAMarcia RiekeSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USAStacey AlbertsSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USAChristina C. WilliamsNSF's National Optical-Infrared Astronomy Research Laboratory, 950 North Cherry Avenue, Tucson, AZ 85719, USAKevin HainlineSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USAFengwu SunSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USADávid PuskásCavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge, CB3 0HE, UKMarianna AnnunziatellaCentro de Astrobiología (CAB), CSIC-INTA, Ctra. de Ajalvir km 4, Torrejón de Ardoz, E-28850, Madrid, SpainWilliam BakerCavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge, CB3 0HE, UKAndrew J. BunkerDepartment of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford, OX1 3RH, UKEiichi EgamiSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USAZhiyuan JiSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USABenjamin D. JohnsonCenter for Astrophysics ∣ Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138 USAB. E. RobertsonDepartment of Astronomy and Astrophysics, University of California, Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USABruno Rodríguez Del PinoCentro de Astrobiología (CAB), CSIC-INTA, Ctra. de Ajalvir km 4, Torrejón de Ardoz, E-28850, Madrid, SpainW. RujopakarnDepartment of Physics, Faculty of Science, Chulalongkorn University, 254 Phayathai Road, Pathumwan, Bangkok 10330, ThailandIrene ShivaeiCentro de Astrobiología (CAB), CSIC-INTA, Ctra. de Ajalvir km 4, Torrejón de Ardoz, E-28850, Madrid, SpainSandro TacchellaCavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge, CB3 0HE, UKChristopher N. A. WillmerSteward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USAChris J. WillottNRC Herzberg, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada

2024en

ABI

Annotatsiya

Abstract We study 31 little red dots (LRD) detected by JADES/NIRCam and covered by the SMILES/MIRI survey, of which ∼70% are detected in the two bluest MIRI bands and 40% in redder MIRI filters. The median/quartiles redshifts are <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>z</mml:mi> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>6.9</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>5.9</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>7.7</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> (55% spectroscopic). The spectral slopes flatten in the rest-frame near-infrared, consistent with a 1.6 μ m stellar bump but bluer than direct pure emission from active galactic nuclei (AGN) tori. The apparent dominance of stellar emission at these wavelengths for many LRDs expedites stellar mass estimation: the median/quartiles are <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>log</mml:mi> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⋆</mml:mo> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>9.4</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>9.1</mml:mn> </mml:mrow> <mml:mrow> <mml:mn>9.7</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> . The number density of LRDs is 10 −4.0±0.1 Mpc −3 , accounting for 14% ± 3% of the global population of galaxies with similar redshifts and masses. The rest-frame near-/mid-infrared (2–4 μ m) spectral slope reveals significant amounts of warm dust (bolometric attenuation ∼3–4 mag). Our spectral energy distribution modeling implies the presence of <0.4 kpc diameter knots, heated by either dust-enshrouded OB stars or an AGN producing a similar radiation field, obscured by A ( V ) > 10 mag. We find a wide variety in the nature of LRDs. However, the best-fitting models for many of them correspond to extremely intense and compact starburst galaxies with mass-weighted ages 5–10 Myr, very efficient in producing dust, with their global energy output dominated by the direct (in the flat rest-frame ultraviolet and optical spectral range) and dust-recycled emission from OB stars with some contribution from an obscured AGN (in the infrared).

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DOI: 10.3847/1538-4357/ad38bb

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