The ongoing hunt for supermassive black hole binaries Jessie Runnoe - - PowerPoint PPT Presentation

▶
the ongoing hunt for supermassive black hole binaries
SMART_READER_LITE
LIVE PREVIEW

The ongoing hunt for supermassive black hole binaries Jessie Runnoe - - PowerPoint PPT Presentation

Aug 18, 2023 298 likes •472 views

Farris et al. (2014) The ongoing hunt for supermassive black hole binaries Jessie Runnoe Black Holes in Dense Star Clusters January 17-22, 2015 - Aspen Center For Physics Collaborators: Gavin Mathes, Michael Eracleous, Todd Boroson,

slide-1
SLIDE 1

The ongoing hunt for supermassive black hole binaries

Jessie Runnoe

Farris et al. (2014)

Collaborators: Gavin Mathes, Michael Eracleous, Todd Boroson, Jules Halpern, Steinn Sigurðsson, Tamara Bogdanović, Alison Pennell

Black Holes in Dense Star Clusters January 17-22, 2015 - Aspen Center For Physics

slide-2
SLIDE 2

The hypothesis: two black holes in a disk

Cuadra et al. (2009)

slide-3
SLIDE 3

The hypothesis: two black holes in a disk

Cuadra et al. (2009)

4600 4700 4800 4900 5000 5100 5200 Rest Wavelength [Å] 50 100 150 200 250 f [1017 erg s1 cm2 Å1]

u2 =

slide-4
SLIDE 4

The binary candidates

  • 88 Type I active galactic nuclei
  • 0.1 < z < 0.7

Velocity (km s-1) Relative fλ Eracleous et al. (2012)

slide-5
SLIDE 5

Project outline

  • Continue spectroscopic monitoring observations
  • Measure velocity variations
  • Check for monotonic velocity changes
  • Compare spectral variability properties to regular quasars
  • Ensemble flux variability
  • Profile variability
  • Optical imaging
  • Look for galaxy interactions.
  • Radio imaging
  • Simulations of the population of binary properties
  • Spectroscopic test for perturbed accretion disks
  • Involves comparison of Balmer and Lyman profiles
slide-6
SLIDE 6

Project outline

  • Continue spectroscopic monitoring observations
  • Measure velocity variations
  • Check for monotonic velocity changes
  • Compare spectral variability properties to regular quasars
  • Ensemble flux variability
  • Profile variability
  • Optical imaging
  • Look for galaxy interactions.
  • Radio imaging
  • Simulations of the population of binary properties
  • Spectroscopic test for perturbed accretion disks
  • Involves comparison of Balmer and Lyman profiles
slide-7
SLIDE 7

Spectroscopic monitoring campaign

  • Multiple follow-up observations


Dec 2009 - Sep 2014 MDM 2.4m Hiltner APO ARC 3.5m KPNO 4m Mayall Palomar 5m Hale 9.2m Hobby-Eberly

2 4 6 8 10 12 14 Observedframe time interval [years] 000 005 010 015 020 025 030 035 040 045 050 055 060 065 070 075 080 085 BBH object number

MDM APO KPNO Palomar HET MDM APO KPNO Palomar HET

slide-8
SLIDE 8

Shifts via cross-correlation analysis

slide-9
SLIDE 9

The radial velocity curve

2000 1000

  • 1000
  • 2000
  • 3000

5 10 15 Hβ radial velocity [km s-1] Rest-frame time [years]

5 10 15

  • 3000

2000 1000 1000 2000

  • J125809

BBH044

slide-10
SLIDE 10

Radial velocity results

  • Eracleous et al. (2012)
  • Mathes et al. (2014 AAS)
  • New spectra

5 10 15

  • 3000

2000 1000 1000 2000 radial velocity [km s ]

J115158 BBH011

5 10 15

  • 3000

2000 1000 1000 2000

  • J001224

BBH026

5 10 15

  • 3000

2000 1000 1000 2000

  • J161911

BBH028

5 10 15 Restframe time [years] 3000 2000 1000 1000 2000 H radial velocity [km s ]

J095539 BBH033

5 10 15 Restframe time [years] 3000 2000 1000 1000 2000

  • J162914

BBH044

5 10 15 Restframe time [years] 3000 2000 1000 1000 2000

  • J123001

BBH075

5 10 15

  • 3000

2000 1000 1000 2000

  • J113706

BBH023

Hβ radial velocity [km s-1] Rest-frame time [years]

slide-11
SLIDE 11

A comparison sample of regular quasars

5 10 15 20

Binary candidates

0.0 0.2 0.4 0.6 0.8 Redshift 10 20 30

Comparison sample

Number of objects 5 10 15 20 25

Binary candidates

43.0 43.5 44.0 44.5 45.0 log(L 5100 Å) [erg s1] 20 40 60

Comparison sample

Number of objects

  • 211 Type I active galactic nuclei
  • multiple epochs of spectroscopy in SDSS
slide-12
SLIDE 12

Hβ flux variability

SDSS quasars Binary candidates

10 100 1000 Restframe time lag [days] 0.1 1.0 H SFIQR [mag]

slide-13
SLIDE 13

Characterizing profile variability

2 2 4 6 8 f [1017 erg s1 cm2 Å1] 4600 4700 4800 4900 5000 5100 5200 Rest Wavelength [Å] 0.0 0.5 1.0 1.5 2.0 Flux ratio 2 2 4 6 8 10 f [1017 erg s1 cm2 Å1] 4600 4700 4800 4900 5000 5100 5200 Rest Wavelength [Å] 0.0 0.5 1.0 1.5 2.0 Flux ratio

χ2=13.7, profile varied χ/nu2=0.03, no profile variability Compare spectra from two epochs. How well does a line fit the ratio spectrum?

slide-14
SLIDE 14

Profile variability results

20 40 60

Binary candidates

5 10 15 20 Reduced 2 100 200 300

Comparison sample

Number of objects

slide-15
SLIDE 15

Up next: a look at the host galaxies

J113651.66+445016.4 J143123.52+392501.4

slide-16
SLIDE 16

The End.