Single-lens mass measurement in the high-magnification microlensing event Gaia19bld located in the Galactic disc

Rybicki, K.; Wyrzykowski, Ł.; Bachelet, E.; Cassan, A.; al.,

doi:10.1051/0004-6361/202039542

Cited by 11 publications

(4 citation statements)

References 88 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The former estimate is empirically confirmed by the derived event rate found by OGLE in their low-cadence Galactic plane survey fields (Mróz et al 2020b). Additional low-cadence (few days) surveys search and detect Galactic-plane microlensing events, e.g., ZTF (Mróz et al 2020a) and Gaia (Wyrzykowski et al 2020;Rybicki et al 2022). A low-cadence Galactic plane survey was also proposed to be conducted with the Vera C. Rubin Observatory (e.g., Gould 2013;Street et al 2018;Sajadian & Poleski 2019), although its survey strategy has not been finalized yet.…”

Section: Microlensingmentioning

confidence: 52%

The Large Array Survey Telescope—Science Goals

Ben-Ami

et al. 2023

PASP

Self Cite

View full text Add to dashboard Cite

The Large Array Survey Telescope (LAST) is designed to survey the variable and transient sky at high temporal cadence. The array is comprised of 48 F/2.2 telescopes of 27.9 cm aperture, coupled to full-frame backside-illuminated cooled CMOS detectors with 3.76 μm pixels, resulting in a pixel scale of 1.″25. A single telescope with a field of view of 7.4 deg2 reaches a 5σ limiting magnitude of 19.6 in 20 s. LAST 48 telescopes are mounted on 12 independent mounts—a modular design which allows us to conduct optimized parallel surveys. Here we provide a detailed overview of the LAST survey strategy and its key scientific goals. These include the search for gravitational-wave (GW) electromagnetic counterparts with a system that can cover the uncertainty regions of the next-generation GW detectors in a single exposure, the study of planetary systems around white dwarfs, and the search for near-Earth objects. LAST is currently being commissioned, with full scientific operations expected in mid 2023. This paper is accompanied by two complementary publications in this issue, giving an overview of the system and of the dedicated data reduction pipeline.

show abstract

Section: Microlensingmentioning

confidence: 52%

The Large Array Survey Telescope—Science Goals

Ben-Ami

et al. 2023

PASP

Self Cite

View full text Add to dashboard Cite

show abstract

“…The potential of microlensing for determining trigonometric parallaxes is also worth mentioning. As recently demonstrated by Rybicki et al (2022), an intensive photometric follow-up of the microlensing event Gaia19bld allowed not only to compute the lens mass but also to derive its distance with a 10% accuracy. Operating in continuous observing mode, RAFTER can provide dense coverage of brightness variation during a microlensing event to find lens properties from photometric data, in addition to the astrometric effect described by Equations (2) to (5).…”

Section: General Relativity and Cosmology-related Experimentsmentioning

confidence: 92%

Relative Astrometry in an Annular Field

Gai

Vecchiato

Riva

et al. 2022

PASP

View full text Add to dashboard Cite

Background. Relative astrometry at or below the microarcsec level with a 1 m class space telescope has been repeatedly proposed as a tool for exo-planet detection and characterization, as well as for several topics at the forefront of Astrophysics and Fundamental Physics. Aim. This paper investigates the potential benefits of an instrument concept based on an annular field of view, as compared to a traditional focal plane imaging a contiguous area close to the telescope optical axis. Method. Basic aspects of relative astrometry are reviewed as a function of the distribution on the sky of reference stars brighter than G = 12 mag (from Gaia EDR3). Statistics of field stars for targets down to G = 8 mag is evaluated by analysis and simulation. Results. Observation efficiency benefits from prior knowledge on individual targets, since source model is improved with few measurements. Dedicated observations (10–20 hr) can constrain the orbital inclination of exoplanets to a few degrees. Observing strategy can be tailored to include a sample of stars, materialising the reference frame, sufficiently large to average down the residual catalog errors to the desired microarcsec level. For most targets, the annular field provides typically more reference stars, by a factor four to seven in our case, than the conventional field. The brightest reference stars for each target are up to 2 mag brighter. Conclusions. The proposed annular field telescope concept improves on observation flexibility and/or astrometric performance with respect to conventional designs. It appears therefore as an appealing contribution to optimization of future relative astrometry missions.

show abstract

“…δ is scaled by θ E and has a maximum amplitude of ≈0.354θ E at | | = u 2 or at u 0 for events with > u 2 0 differing from the characteristics of photometric microlensing. In photometric microlensing, the amplification can increase almost arbitrarily for arbitrarily close lens-source impact parameters and is only eventually bounded by finite-source effects (e.g., Rybicki et al 2022)…”

Section: Astrometric Microlensingmentioning

confidence: 99%

Astrometric Microlensing by Primordial Black Holes with the Roman Space Telescope

Fardeen,

McGill,

Perkins

et al. 2024

ApJ

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

Single-lens mass measurement in the high-magnification microlensing event Gaia19bld located in the Galactic disc

Cited by 11 publications

References 88 publications

The Large Array Survey Telescope—Science Goals

The Large Array Survey Telescope—Science Goals

Relative Astrometry in an Annular Field

Astrometric Microlensing by Primordial Black Holes with the Roman Space Telescope

Contact Info

Product

Resources

About