<i>HST</i>
                    Imaging of MEGA Microlensing Candidates in M31

Cseresnjes, P.; Crotts, Arlin; Jong, J. T. A. de; Bergier, Alex; Baltz, Edward A.; Gyuk, G.; Kuijken, Konrad; Widrow, Lawrence M.

doi:10.1086/498501

Cited by 6 publications

(5 citation statements)

References 21 publications

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“…Knowledge of the total mass of M31 is vital for the interpretation of the latest generation of pixel microlensing experiments, which concentrate on that galaxy (Crotts 1992; Kerins et al 2001, 2003; Riffeser et al 2003; de Jong et al 2004; Belokurov et al 2005; Cseresnjes et al 2005). Evans & Wilkinson (2000) have found that there is no kinematic evidence to support the widely held belief that M31 is more massive than the Milky Way, in contradiction to previous studies.…”

Section: Introductioncontrasting

confidence: 99%

Planetary nebula velocities in the disc and bulge of M31

Halliday¹,

Carter²,

Bridges³

et al. 2006

Monthly Notices of the Royal Astronomical Society

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We present radial velocities for a sample of 723 planetary nebulae in the disc and bulge of M31, measured using the WYFFOS fibre spectrograph on the William Herschel Telescope. Velocities are determined using the [O iii] λ5007 emission line. Rotation and velocity dispersion are measured to a radius of 50 arcmin (11.5 kpc), the first stellar rotation curve and velocity dispersion profile for M31 to such a radius. Our kinematics are consistent with rotational support at radii well beyond the bulge effective radius of 1.4 kpc, although our data beyond a radius of 5 kpc are limited. We present tentative evidence for kinematic substructure in the bulge of M31 to be studied fully in a later work. This paper is part of an ongoing project to constrain the total mass, mass distribution and velocity anisotropy of the disc, bulge and halo of M31.

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Section: Introductioncontrasting

confidence: 99%

Planetary nebula velocities in the disc and bulge of M31

Halliday¹,

Carter²,

Bridges³

et al. 2006

Monthly Notices of the Royal Astronomical Society

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“…Its short duration, good sampling and probed achromaticity make of it a robust microlensing event. Furthermore, the possible source has been identified on some HST frame (this identification, however, has been challenged by Cseresnjes et al [96]). PA-N2 [45]/MEGA-ML7 [38], Fig.…”

Section: The Microlensing Candidate Eventsmentioning

confidence: 99%

Pixel lensing

Novati

2009

Gen Relativ Gravit

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Pixel lensing is gravitational microlensing of unresolved stars. The main target explored up to now has been the nearby galaxy of Andromeda, M31. The scientific issues of interest are the search for dark matter in form of compact halo objects, the study of the characteristics of the luminous lens and source populations and the possibility of detecting extra-solar (and extra-galactic) planets. In the present work we intend to give an updated overview of the observational status in this field.

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“…With the source magnitude and color fixed thanks to an analysis of archival Hubble Space Telescope (HST) data, and based on a specific Monte Carlo simulation of the experiment, where the observed characteristics of the event had been used to delimit the possible parameter space (using in particular a lower limit for the lens proper motion), Aurière et al (2001) conclude that the PA-N1 lens is more likely a MACHO if the mass halo fraction in the form of compact halo object is above 20%. The results of this analysis have been however challenged by the MEGA collaboration (who also reported this event as MEGA-ML16, de Jong et al 2006), in particular by Cseresnjes et al (2005) who argued, on the basis of new HST observations, against the source identification reported in Aurière et al (2001).…”

Section: Introductionmentioning

confidence: 98%

M31 Pixel Lensing Event Oab-N2: A Study of the Lens Proper Motion

Novati

Dall’Ora

Gould

et al. 2010

ApJ

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We present an updated analysis of the M31 pixel lensing candidate event OAB-N2 previously reported in Calchi . Here we take advantage of new data both astrometric and photometric. Astrometry: using archival 4m-KPNO and HST/WFPC2 data we perform a detailed analysis on the event source whose result, although not fully conclusive on the source magnitude determination, is confirmed by the following light curve photometry analysis. Photometry: first, unpublished WeCAPP data allows us to confirm OAB-N2, previously reported only as a viable candidate, as a well constrained pixel lensing event. Second, this photometry enables a detailed analysis in the event parameter space including the effects due to finite source size. The combined results of these analyses allow us to put a strong lower limit on the lens proper motion. This outcome favors the MACHO lensing hypothesis over self lensing for this individual event and points the way toward distinguishing between the MACHO and self-lensing hypotheses from larger data sets.

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HST Imaging of MEGA Microlensing Candidates in M31

Cited by 6 publications

References 21 publications

Planetary nebula velocities in the disc and bulge of M31

Planetary nebula velocities in the disc and bulge of M31

Pixel lensing

M31 Pixel Lensing Event Oab-N2: A Study of the Lens Proper Motion

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