Large-Scale Searches for Brown Dwarfs and Free-Floating Planets

Burningham, B.

doi:10.1007/978-3-319-30648-3_118-1

Cited by 3 publications

(3 citation statements)

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“…Brown dwarfs (hereafter BDs) are by definition bodies that are not massive enough to fuse hydrogen in their interior stably, but are massive enough to undergo a brief phase of deuterium burn-Article number, page 2 of 16 ing soon after their formation. The very first two BDs were discovered in 1995 (Nakajima et al 1995;Rebolo et al 1995), and today over 1000 BDs have been detected in the solar neighbourhood (Burningham 2018). Some of these objects have also been discovered around single WDs.…”

Section: Brown Dwarfsmentioning

confidence: 99%

Circumbinary exoplanets and brown dwarfs with the Laser Interferometer Space Antenna

Danielski

Korol

Rossi

2019

A&A

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Aims. We explore the prospects for the detection of giant circumbinary exoplanets and brown dwarfs (BDs) orbiting Galactic double white dwarfs binaries (DWDs) with the Laser Interferometer Space Antenna (LISA). Methods. By assuming an occurrence rate of 50%, motivated by white dwarf pollution observations, we built a Galactic synthetic population of P-type giant exoplanets and BDs orbiting DWDs. We carried this out by injecting different sub-stellar populations, with various mass and orbital separation characteristics, into the DWD population used in the LISA mission proposal. We then performed a Fisher matrix analysis to measure how many of these three-body systems show a periodic Doppler-shifted gravitational wave perturbation detectable by LISA. Results. We report the number of circumbinary planets (CBPs) and (BDs) that can be detected by LISA for various combinations of mass and semi-major axis distributions. We identify pessimistic and optimistic scenarios corresponding, respectively, to 3 and 83 (14 and 2218) detections of CBPs (BDs), observed during the length of the nominal LISA mission. These detections are distributed all over the Galaxy following the underlying DWD distribution, and they are biased towards DWDs with higher LISA signal-to-noise ratio and shorter orbital period. Finally, we show that if LISA were to be extended for four more years, the number of systems detected will be more than doubled in both the optimistic and pessimistic scenarios. Conclusions. Our results present promising prospects for the detection of post-main sequence exoplanets and BDs, showing that gravitational waves can prove the existence of these populations over the totality of the Milky Way. Detections by LISA will deepen our knowledge on the life of exoplanets subsequent to the most extreme evolution phases of their hosts, clarifying whether new phases of planetary formation take place later in the life of the stars. Such a method is strongly complementary to electromagnetic studies within the solar region and opens a window into the investigation of planets and BDs everywhere in the entire Galaxy, and possibly even in nearby galaxies in the Local Group. Evidences for sub-stellar objects around WDs White dwarf pollutionWhite dwarfs are expected to have a pure H or He atmosphere (Schatzman 1945) and their high surface gravity (∼ 10 5 denser than the Sun) makes the sinking metals diffusion timescale several order of magnitude shorter than the evolutionary period. Yet, observations show the presence of heavy elements in the spectra of 25% to 50% of all observed WDs (Zuckerman et al. 2003(Zuckerman et al. , 2010Koester et al. 2014), indicating that a continuous supply Article number, page 1 of 16

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Section: Brown Dwarfsmentioning

confidence: 99%

Circumbinary exoplanets and brown dwarfs with the Laser Interferometer Space Antenna

Danielski

Korol

Rossi

2019

A&A

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“…After D and Li exhaustion, an inert BD can be conceived as a remnant in the aforementioned sense. For further details, an interested reader is addressed to review papers e.g., [17] [22] or research articles e.g., [20] [21] [103] [12] [19].…”

Section: Stellar Remnantsmentioning

confidence: 99%

On the desert between neutron star and black hole remnants

Caimmi¹

2018

ams

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The occurrence of a desert between neutron star (NS) and black hole (BH) remnants is reviewed using a set of well-determined masses from different sources. The dependence of stellar remnants on the zero age main sequence (ZAMS) progenitor mass for solar metallicity is taken from a recent investigation and further effort is devoted to NS and BH remnants. In particular, a density parameter is defined and related to NS mass and radius. Spinning BHs in Kerr metrics are considered as infinitely thin, homogeneous, rigidly rotating disks in Newtonian mechanics. Physical parameters for nonrotating (TOV) and equatorial breakup (EQB) configurations are taken or inferred from a recent investigation with regard to 4 NS and 3 quark star (QS) physically motivated equation of state (EOS) kinds. A comparison is performed with counterparts related to nonrotating and maximally rotating BHs. The results are also considered in the light of empirical relations present in literature. With regard to J-M relation, EQB configurations are placed on a sequence of similar slope in comparison to maximally rotating BHs, but shifted downwards due to lower angular momentum by a factor of about 3.6. Under the assumption heavy baryons are NS constituents and instantaneously undergo quark-level reactions, the energy released (or adsorbed) is calculated using results from a recent investigation. Even if NSs exclusively host heavy baryons of the kind considered, the total amount cannot exceed about 10% of the binding energy, which inhibits supernova explosions as in supramassive white dwarf (WD) remnants or implosions into BH. Alternative channels for submassive (2 < ∼ M/m ⊙ < ∼ 4) BH formation are shortly discussed. Whether the desert between NS and BH remnants could be ascribed to biases and/or selection effects, or related to lack of formation channels, still remains an open question. To this respect, increasingly refined theoretical and observational techniques are needed.keywords -stars: evolution -stellar remnants -nucleosynthesisneutron stars -black holes.

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“…Indeed, WISE has already established the existence of a new brown dwarf spectral class with T eff 500 K (Y dwarfs; Cushing et al 2011;Kirkpatrick et al 2011). Although prior WISE brown dwarf searches have been highly successful (e.g., Cushing et al 2011;Kirkpatrick et al 2011Kirkpatrick et al , 2012Griffith et al 2012;Mace et al 2013a;Luhman 2014a;Kirkpatrick et al 2014Kirkpatrick et al , 2016Pinfield et al 2014a;Schneider et al 2016;Kuchner et al 2017;Tinney et al 2018;Burningham 2018), the Y dwarf census has stagnated in recent years at a sample size of just ∼25-30 objects.…”

Section: Introductionmentioning

confidence: 99%

Expanding the Y Dwarf Census with Spitzer Follow-up of the Coldest CatWISE Solar Neighborhood Discoveries

Meisner

Caselden

Kirkpatrick

et al. 2020

ApJ

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We present Spitzer 3.6µm and 4.5µm follow-up of 170 candidate extremely cool brown dwarfs newly discovered via the combination of WISE and NEOWISE imaging at 3−5µm. CatWISE, a joint analysis of archival WISE and NEOWISE data, has improved upon the motion measurements of AllWISE by leveraging a >10× time baseline enhancement, from 0.5 years (AllWISE) to 6.5 years (CatWISE). As a result, CatWISE motion selection has yielded a large sample of previously unrecognized brown dwarf candidates, many of which have archival detections exclusively in the WISE 4.6µm (W2) channel, suggesting that they could be both exceptionally cold and nearby. Where these objects go undetected in WISE W1 (3.4µm), Spitzer can provide critically informative detections at 3.6µm. Of our motionconfirmed discoveries, seventeen have a best-fit Spitzer [3.6]−[4.5] color most consistent with spectral type Y. CWISEP J144606.62−231717.8 (µ ≈ 1.3 ′′ /yr) is likely the reddest, and therefore potentially coldest, member of our sample with a very uncertain [3.6]−[4.5] color of 3.71 ± 0.44 magnitudes. We also highlight our highest proper motion discovery, WISEA J153429.75−104303.3, with µ ≈ 2.7 ′′ /yr. Given that the prior list of confirmed and presumed Y dwarfs consists of just 27 objects, the Spitzer follow-up presented in this work has substantially expanded the sample of identified Y dwarfs. Our new discoveries thus represent significant progress toward understanding the bottom of the substellar mass function, investigating the diversity of the Y dwarf population, and selecting optimal brown dwarf targets for JWST spectroscopy.

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Large-Scale Searches for Brown Dwarfs and Free-Floating Planets

Cited by 3 publications

References 135 publications

Circumbinary exoplanets and brown dwarfs with the Laser Interferometer Space Antenna

Circumbinary exoplanets and brown dwarfs with the Laser Interferometer Space Antenna

On the desert between neutron star and black hole remnants

Expanding the Y Dwarf Census with Spitzer Follow-up of the Coldest CatWISE Solar Neighborhood Discoveries

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