Maqola

Tidal Disruption Event Demographics with the Zwicky Transient Facility: Volumetric Rates, Luminosity Function, and Implications for the Local Black Hole Mass Function

Yuhan YaoMiller Institute for Basic Research in Science, 468 Donner Lab, Berkeley, CA 94720, USAVikram RaviCahill Center for Astrophysics, California Institute of Technology, MC 249-17, 1200 E California Boulevard, Pasadena, CA 91125, USASuvi GezariSpace Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USASjoert van VelzenLeiden Observatory, Leiden University, Postbus 9513, 2300 RA, Leiden, The NetherlandsWenbin LuDepartment of Astronomy, University of California, Berkeley, CA 94720, USAS. SchulzeDepartment of Physics, The Oskar Klein Centre, Stockholm University, AlbaNova, SE-10691 Stockholm, SwedenJean J. SomalwarCahill Center for Astrophysics, California Institute of Technology, MC 249-17, 1200 E California Boulevard, Pasadena, CA 91125, USAS. R. KulkarniCahill Center for Astrophysics, California Institute of Technology, MC 249-17, 1200 E California Boulevard, Pasadena, CA 91125, USAErica HammersteinDepartment of Astronomy, University of Maryland, College Park, MD 20742, USAM. NichollBirmingham Institute for Gravitational Wave Astronomy and School of Physics and Astronomy, University of Birmingham, Birmingham B15 2TT, UKM. J. GrahamCahill Center for Astrophysics, California Institute of Technology, MC 249-17, 1200 E California Boulevard, Pasadena, CA 91125, USAD. A. PerleyAstrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UKS. B. CenkoJoint Space-Science Institute, University of Maryland, College Park, MD 20742, USARobert SteinCahill Center for Astrophysics, California Institute of Technology, MC 249-17, 1200 E California Boulevard, Pasadena, CA 91125, USAAngelo RicarteCenter for Astrophysics ∣ Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USAUrmila ChadayammuriCenter for Astrophysics ∣ Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USAEliot QuataertDepartment of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USAE. BellmDIRAC Institute, Department of Astronomy, University of Washington, 3910 15th Avenue NE, Seattle, WA 98195, USAJ. S. BloomDepartment of Astronomy, University of California, Berkeley, CA 94720, USARichard DekanyCaltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USAA. J. DrakeCahill Center for Astrophysics, California Institute of Technology, MC 249-17, 1200 E California Boulevard, Pasadena, CA 91125, USASteven L. GroomIPAC, California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125, USAAshish A MahabalCenter for Data Driven Discovery, California Institute of Technology, Pasadena, CA 91125, USAThomas A. PrinceCahill Center for Astrophysics, California Institute of Technology, MC 249-17, 1200 E California Boulevard, Pasadena, CA 91125, USAReed RiddleCaltech Optical Observatories, California Institute of Technology, Pasadena, CA 91125, USABen RusholmeIPAC, California Institute of Technology, 1200 E. California Blvd, Pasadena, CA 91125, USAY. SharmaCahill Center for Astrophysics, California Institute of Technology, MC 249-17, 1200 E California Boulevard, Pasadena, CA 91125, USAJ. SollermanDepartment of Astronomy, The Oskar Klein Centre, Stockholm University, AlbaNova, SE-10691 Stockholm, SwedenLin YanCahill Center for Astrophysics, California Institute of Technology, MC 249-17, 1200 E California Boulevard, Pasadena, CA 91125, USA

2023en

ABI

Annotatsiya

Abstract We conduct a systematic tidal disruption event (TDE) demographics analysis using the largest sample of optically selected TDEs. A flux-limited, spectroscopically complete sample of 33 TDEs is constructed using the Zwicky Transient Facility over 3 yr (from 2018 October to 2021 September). We infer the black hole (BH) mass ( M BH ) with host galaxy scaling relations, showing that the sample M BH ranges from 10 5.1 M ⊙ to 10 8.2 M ⊙ . We developed a survey efficiency corrected maximum volume method to infer the rates. The rest-frame g -band luminosity function can be well described by a broken power law of <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>ϕ</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>g</mml:mi> </mml:mrow> </mml:msub> <mml:mo stretchy="false">)</mml:mo> <mml:mo>∝</mml:mo> <mml:msup> <mml:mrow> <mml:mfenced close="]" open="["> <mml:mrow> <mml:msup> <mml:mrow> <mml:mfenced close=")" open="("> <mml:mrow> <mml:msub> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>g</mml:mi> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:msub> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>bk</mml:mi> </mml:mrow> </mml:msub> </mml:mrow> </mml:mfenced> </mml:mrow> <mml:mrow> <mml:mn>0.3</mml:mn> </mml:mrow> </mml:msup> <mml:mo>+</mml:mo> <mml:msup> <mml:mrow> <mml:mfenced close=")" open="("> <mml:mrow> <mml:msub> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>g</mml:mi> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:msub> <mml:mrow> <mml:mi>L</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>bk</mml:mi> </mml:mrow> </mml:msub> </mml:mrow> </mml:mfenced> </mml:mrow> <mml:mrow> <mml:mn>2.6</mml:mn> </mml:mrow> </mml:msup> </mml:mrow> </mml:mfenced> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> </mml:math> , with L bk = 10 43.1 erg s −1 . In the BH mass regime of 10 5.3 ≲ ( M BH / M ⊙ ) ≲ 10 7.3 , the TDE mass function follows <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>ϕ</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>BH</mml:mi> </mml:mrow> </mml:msub> <mml:mo stretchy="false">)</mml:mo> <mml:mo>∝</mml:mo> <mml:msubsup> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>BH</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.25</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> , which favors a flat local BH mass function ( <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi mathvariant="italic">dn</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>BH</mml:mi> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:mi>d</mml:mi> <mml:mi>log</mml:mi> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mi>BH</mml:mi> </mml:mrow> </mml:msub> <mml:mo>≈</mml:mo> <mml:mi>constant</mml:mi> </mml:math> ). We confirm the significant rate suppression at the high-mass end ( M BH ≳ 10 7.5 M ⊙ ), which is consistent with theoretical predictions considering direct capture of hydrogen-burning stars by the event horizon. At a host galaxy mass of M gal ∼ 10 10 M

Hali tarjima qilinmagan

Identifikatorlar

DOI: 10.3847/2041-8213/acf216

Iqtiboslar va manbalar

2 ta iqtibos0 ta foydalanilgan manba

Koʻrsatkichlar — AkademScholar