A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191

Lam, Casey Y.; Lu, Jessica R.

doi:10.3847/1538-4357/aced4a

Cited by 10 publications

(4 citation statements)

References 29 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…An isolated stellar-mass BH has recently been detected and characterized with microlensing, using ground-based survey photometry and Hubble Space Telescope follow-up astrometry (Lam et al 2022;Mróz et al 2022;Sahu et al 2022;Lam & Lu 2023). This BH lens has been used to constrain the properties of natal kicks (Andrews & Kalogera 2022) as well as whether the progenitor system was binary or single (Vigna-Gómez & Ramirez-Ruiz 2023).…”

Section: Distinguishing Between Kick Prescriptions With Gravitational...mentioning

confidence: 99%

Natal Kicks from the Galactic Center and Implications on Their Environment and for the Nancy Grace Roman Space Telescope

Jurado,

Naoz,

Lam

et al. 2024

ApJ

View full text Add to dashboard Cite

Most galaxies, including the Milky Way, harbor a central supermassive black hole (SMBH) weighing millions to billions of solar masses. Surrounding these SMBHs are dense regions of stars and stellar remnants, such as neutron stars (NSs) and black holes (BHs). NSs and possibly BHs receive large natal kicks at birth on the order of hundreds of kilometers per second. The natal kicks that occur in the vicinity of an SMBH may redistribute the orbital configuration of the compact objects and alter their underlying density distribution. We model the effects of natal kicks on a Galactic center (GC) population of massive stars and stellar binaries with different initial density distributions. Using observational constraints from stellar orbits near the GC, we place an upper limit on the steepness of the initial stellar profile and find it to be core-like. In addition, we predict that 30%–70% of compact objects become unbound from the SMBH due to their kicks and will migrate throughout the Galaxy. Different BH kick prescriptions lead to distinct spatial and kinematic distributions. We suggest that the Nancy Grace Roman Space Telescope may be able to distinguish between these distributions and thus be able to differentiate between natal kick mechanisms.

show abstract

Section: Distinguishing Between Kick Prescriptions With Gravitational...mentioning

confidence: 99%

Natal Kicks from the Galactic Center and Implications on Their Environment and for the Nancy Grace Roman Space Telescope

Jurado,

Naoz,

Lam

et al. 2024

ApJ

View full text Add to dashboard Cite

show abstract

“…Although these astrometric and photometric signals arise from the same underlying phenomena, their characteristics, and information content differ (e.g., Dominik & Sahu 2000;Belokurov & Evans 2002). Notably, unlike the photometric signal, the detection of the astrometric signal can lead to lensmass determinations (Lu et al 2016;Sahu et al 2017;Zurlo et al 2018;Lam et al 2022;Sahu et al 2022;Lam & Lu 2023;McGill et al 2023). Overall, photometric and astrometric microlensing signals can offer complementary probes and are sensitive to different lens mass-distance configurations (Dominik & Sahu 2000).…”

Section: Introductionmentioning

confidence: 99%

Astrometric Microlensing by Primordial Black Holes with the Roman Space Telescope

Fardeen,

McGill,

Perkins

et al. 2024

ApJ

Self Cite

View full text Add to dashboard Cite

Primordial black holes (PBHs) could explain some fraction of dark matter and shed light on many areas of early-Universe physics. Despite over half a century of research interest, a PBH population has so far eluded detection. The most competitive constraints on the fraction of dark matter comprised of PBHs (f DM) in the (10−9–10)M ⊙ mass ranges come from photometric microlensing and bound f DM ≲ 10−2–10−1. With the advent of the Roman Space Telescope with its submilliarcsecond astrometric capabilities and its planned Galactic Bulge Time Domain Survey (GBTDS), detecting astrometric microlensing signatures will become routine. Compared with photometric microlensing, astrometric microlensing signals are sensitive to different lens masses–distance configurations and contain different information, making it a complimentary lensing probe. At submilliarcsecond astrometric precision, astrometric microlensing signals are typically detectable at larger lens–source separations than photometric signals, suggesting a microlensing detection channel of pure astrometric events. We use a Galactic simulation to predict the number of detectable microlensing events during the GBTDS via this pure astrometric microlensing channel. Assuming an absolute astrometric precision floor for bright stars of 0.1 mas for the GBTDS, we find that the number of detectable events peaks at ≈103 f DM for a population of 1M ⊙ PBHs and tapers to ≈10f DM and ≈100f DM at 10−4 M ⊙ and 103 M ⊙, respectively. Accounting for the distinguishability of PBHs from stellar lenses, we conclude the GBTDS will be sensitive to a PBH population at f DM down to ≈10−1–10−3 for (10−1–102)M ⊙ likely yielding novel PBH constraints.

show abstract

“…Although challenging to discover, microlensing events are scientifically valuable as they provide the means to measure the masses of objects that would otherwise be too faint to observe, including free-floating planets (Gould et al 2022;Koshimoto et al 2023;Sumi et al 2023), and even isolated compact objects such as black holes and neutron stars (Sahu et al 2022;Lam & Lu 2023). Planetary, Brown Dwarf and stellar companions of lensing stars can betray their presence by causing short-lived (∼hours-days) "anomalous" deviations to the otherwise-smooth lensing light curve (Mao & Paczynski 1991).…”

Section: Introductionmentioning

confidence: 99%

ROME/REA: Three-year, Tri-color Timeseries Photometry of the Galactic Bulge

Street,

Bachelet,

Tsapras

et al. 2024

PASP

View full text Add to dashboard Cite

The Robotic Observations of Microlensing Events/Reactive Event Assessment Survey was a Key Project at Las Cumbres Observatory (hereafter LCO) which continuously monitored 20 selected fields (3.76 sq.deg) in the Galactic Bulge throughout their seasonal visibility window over a three-year period, between 2017 March and 2020 March. Observations were made in three optical passbands (SDSS − g ′ , − r ′ , − i ′ ), and LCO’s multi-site telescope network enabled the survey to achieve a typical cadence of ∼10 hr in i ′ and ∼15 hr in g ′ and r ′ . In addition, intervals of higher cadence (<1 hr) data were obtained during monitoring of key microlensing events within the fields. This paper describes the Difference Image Analysis data reduction pipeline developed to process these data, and the process for combining the photometry from LCO’s three observing sites in the Southern Hemisphere. The full timeseries photometry for all ∼8 million stars, down to a limiting magnitude of i ∼ 18 mag is provided in the data release accompanying this paper, and samples of the data are presented for exemplar microlensing events, illustrating how the tri-band data are used to derive constraints on the microlensing source star parameters, a necessary step in determining the physical properties of the lensing object. The timeseries data also enables a wealth of additional science, for example in characterizing long-timescale stellar variability, and a few examples of the data for known variables are presented.

show abstract

A Reanalysis of the Isolated Black Hole Candidate OGLE-2011-BLG-0462/MOA-2011-BLG-191

Cited by 10 publications

References 29 publications

Natal Kicks from the Galactic Center and Implications on Their Environment and for the Nancy Grace Roman Space Telescope

Natal Kicks from the Galactic Center and Implications on Their Environment and for the Nancy Grace Roman Space Telescope

Astrometric Microlensing by Primordial Black Holes with the Roman Space Telescope

ROME/REA: Three-year, Tri-color Timeseries Photometry of the Galactic Bulge

Contact Info

Product

Resources

About