Authors: Andy D. Goulding, Kris Pardo, Jenny E. Greene, Chiara M. F. Mingarelli, Kristina Nyland, & Michael A. Strauss
First Author’s Institution: Department of Astrophysical Sciences, Princeton University
Status: Accepted to the Astrophysical Journal Letters, open access on ArXiv
With the announcement of the experimental confirmation of gravitational waves by LIGO in 2016 in tandem with additional electromagnetic follow-up of a neutron star merger, astronomy was quickly ushered into an era of truly multi-messenger science. Although the number of gravitational wave events since observed by LIGO is already substantial, the sheer number of black holes (and neutron stars) predicted to exist within our Universe vastly outweighs this cumulative yield. One reason why LIGO is not constantly finding strong gravitational waves from all of these black holes (the gravitational wave background or GWB) is that not every black hole exists in a pair, which is a necessary condition to spiral inwards, merge, and set off a gravitational wave event. Predictions suggest that the timescales required for some of these events to occur are a sizable fraction of the age of our Universe!
LIGO has however shown direct evidence for the merging of solar mass black holes with atypically large masses between 10 – 40 Msun, and although easier to observe due to their strong gravitational signal, their existence has continued to challenge theoretical explanations. Scaling up to even greater masses does not reduce the pressure on theory either, as the predicted dominant mass contribution to the yet undetected GWB is from super-massive black holes (SMBHs) on the order of 10^8 – 10^9 Msun.
It has long been hypothesized that SMBHs inhabit the central-most regions of almost all galaxies, and accumulative mass through the slow accretion of gas and stellar material. When galaxies undergo the often violent processes of a wholesale merger, these SMBHs are predicted to collect within the central region of a galaxy and become gravitationally bound on short Myr timescales, accelerated by dynamical friction. However, the black hole pair can only bleed off so much energy through interacting with nearby material and at some point within the final parsec the merger is predicted to stall out. This so-called “final parsec problem” has yet to be resolved. For the sample of intermediate-mass black hole mergers suggested by the LIGO observations, it appears that nature has ways around this problem. Whether this is true for SMBH mergers has yet to be seen.
Putting the final parsec problem aside, the authors of today’s astrobite provide definitive evidence for a precursor system which may one day produce a low-frequency gravitational wave event consistent with a strong contribution to the GWB.
As shown in Figure 1, observations with the WFC3 instrument aboard the Hubble Space Telescope revealed a pair of tightly bound SMBH candidates in a highly luminous post-merger galaxy, poetically named “SDSSJ1010+1413”. Accounting for the cosmological distance, the separation between the SMBHs is found to be ~430 pc. Previous studies examining the velocities and dynamics of the galaxy confirm the outward tell-tale signs of a trainwreck galaxy and provide the context for the apparently resolved pair of SMBHs in its core. Special imaging with an appropriate [OIII] narrowband filter corroborates this picture by defining the extent of the extremely luminous [OIII] emission and characteristic ionized gas associated with powerfully accreting SMBHs (AKA quasars). However, coincident X-ray observations with the Chandra Space Telescope showed very little X-ray light which, when compared to infrared estimates, suggest an obscuring cloud of thick gas along the line of sight.
Despite the awesome resolution of the Hubble Space Telescope (~0.04”), such an observation of a supposed SMBH pair may be ambiguous. To increase confidence in this interpretation, the authors modeled each of the sources with a coincident point-like model and an extended Gaussian model. Even so, a single SMBH with extended [OIII] and bisecting obscuration due to a dust lane could mimic this scenario, albeit with a significantly worse fit. Given the former scenario, each SMBH is estimated to have a minimum mass of 4×10^8 Msun based on the Eddington luminosity limit, putting them in the sweet spot of GWB contribution.
Lastly, the authors make tentative predictions for a future low-frequency high-mass gravitational wave event, as shown in Figure 2. By considering carefully motivated arguments for dynamical friction, they surmise a coalescence timescale of 0.1 – 2 Gyr, where the lower limit is argued from the seemingly large gas reservoir near the SMBHs, which may help dissipate energy and rapidly close their orbital separation. Ignoring the ‘last parsec problem’, they argue that once the system reaches < 0.1 pc separation, the gravitational wave emission will enable the pair to finally merge within ~700Myr. Given that the lookback time to this galaxy at z~0.2 is on the order of the predicted merger timescale, this discovery provides strong evidence that such galaxies could be contributing to the GWB right now.
The low-frequency nanohertz GWB signal will not be detectable by current observatories such as LIGO. However, these increasingly powerful facilities will soon be complemented by hyper-sensitive Pulsar Timing Arrays which should be able to detect a nanohertz GWB signal, as may be produced by such a pair of quasars in this and other trainwreck galaxies.