Kelly Holley-Bockelmann, for the NASA LISA Study Team

Athena + LISA = AWESOME

Kelly Holley-Bockelmann, for the NASA LISA Study Team Vanderbilt University and Fisk University Gravitational waves come from a time-dependent mass quadrupole Gravitational waves encode mass, spin, orbit and distance

BBH no spin BBH with spin

For objects with orbital periods of seconds — hours… Imagine what you could do with:

Masses: 0.01 - 1% Distances: 1-10% Spins:1-10% Spin directions: 10 degrees Sky localization: 1 arcmin2 — 10 deg2 Eccentricity:1% Discovery Space Millions of close compact object binaries 47 Tuc X9 — a BH-WD on a 28m orbital period, X-ray bright and (almost) a LISA source

Bahramian et al. 2017

1034

1033 Luminosity0.5-10from (ers/s keV

Combining X-ray and GW data will help improve the mass measurements, allowing us to get a better handle on the accretion physics 47 Tuc X9 — a BH-WD on a 28m orbital period, X-ray bright and (almost) a LISA source

Bahramian et al. 2017 15 10°

16 10°

17 10°

18 10°

19 10° Characteristic Strain 20 10°

21 10°

5 4 3 2 1 0 10° 10° 10° 10° 10° 10 f [Hz]

Combining X-ray and GW data will help improve the mass measurements, allowing us to get a better handle on the accretion physics Mergers of Milky-Way Class Supermassive Black Holes COSMIC DAWN

NEAR FUTURE UVOIR SURVEYS: JWST, LSST

SKA, PULSAR LIGO TIMING LISA detects the inspiral and merger of intermediate mass and Milky Way-class black holes with huge SNR throughout the observable universe and into the Cosmic Dawn. COSMIC DAWN

NEAR FUTURE UVOIR SURVEYS: JWST, LSST

SKA, PULSAR LIGO TIMING

LISA detects the inspiral and merger of intermediate mass and Milky Way-class black holes with huge SNR throughout the observable universe and into the Cosmic Dawn. 3D GRMHD + ray-tracing show periodic UV, extreme UV, and hard X-ray variability at the binary orbital frequency

d’Ascoli et al. 2018

Athena’s wide FOV and TOO capability with few hour leadtime provide a chance to observe a SMBH merger weeks to hours beforehand in X- rays and GWs Flux, for a column density of 1023

Exposure time in ksec Black hole cosmology with

•BH mergers as standard sirens

•chirp rate gives mass

•mass gives intrinsic amplitude

•measured amplitude gives distance

•combine with redshift to get H0

•Need EM follow-up to identify Luminosity distances for simulated (or constrain) hosts catalog of LISA BH binaries (N. Tamanini)

While the theoretical and technological dust settles, let’s think beyond contemporaneous electromagnetic counterparts

Schnittman 2009

For example: Athena would be great to survey the Xray time domain to help with population studies/Bayesian priors for potential binary candidates… Tanks! Want more LISA info? Ask us…or read a white paper:

Natarajan+ — Seed BHs; Bellovary+ — IMBHs; Colpi+ — SMBHs; Caldwell+ — Cosmology; Cornish+ — Discovery; Eracleous+ — TDEs; Berti+ — Fundamental Physics; Berry+ — EMRIs; Baker+ — MMA/LISA; McWIlliams+ — GW Astro; Brown+ — Galactic Binaries; Cutler+ — Multiband GW LISA can peer into the dark ages when black hole seeds are sown