NICMOS Kernel-phase Interferometry. II. Demographics of Nearby Brown Dwarfs

Star formation theories have struggled to reproduce binary brown dwarf population demographics (e.g., frequency, separation, and mass ratio). Kernel-phase interferometry is sensitive to companions at separations inaccessible to classical imaging, enabling tests of these theories at new physical scal...
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Gespeichert in:

Autor*in:	Samuel M. Factor [verfasserIn] Adam L. Kraus [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2023

Schlagwörter:	Brown dwarfs L dwarfs T dwarfs Direct detection interferometry Direct imaging Hubble Space Telescope

Übergeordnetes Werk:	In: The Astronomical Journal - IOP Publishing, 2022, 165(2023), 3, p 130
Übergeordnetes Werk:	volume:165 ; year:2023 ; number:3, p 130

Links:	Link aufrufen Link aufrufen Link aufrufen Journal toc

DOI / URN:	10.3847/1538-3881/aca475

Katalog-ID:	DOAJ089162013

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spelling	10.3847/1538-3881/aca475 doi (DE-627)DOAJ089162013 (DE-599)DOAJ9bffad89f1b440cda889d9dad8a81274 DE-627 ger DE-627 rakwb eng QB1-991 Samuel M. Factor verfasserin aut NICMOS Kernel-phase Interferometry. II. Demographics of Nearby Brown Dwarfs 2023 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Star formation theories have struggled to reproduce binary brown dwarf population demographics (e.g., frequency, separation, and mass ratio). Kernel-phase interferometry is sensitive to companions at separations inaccessible to classical imaging, enabling tests of these theories at new physical scales below the hydrogen burning limit. We analyze the detections and sensitivity limits from our previous kernel-phase analysis of archival HST/NICMOS surveys of field brown dwarfs. After estimating physical properties of the 105 late-M to T dwarfs using Gaia distances and evolutionary models, we use a Bayesian framework to compare these results to a model companion population defined by log-normal separation and power-law mass-ratio distributions. When correcting for Malmquist bias, we find a companion fraction of $F={0.11}_{-0.03}^{+0.04}$ and a separation distribution centered at $\rho ={2.2}_{-1.0}^{+1.2}$ au, smaller and tighter than seen in previous studies. We also find a mass-ratio power-law index that strongly favors equal-mass systems: $\gamma ={4.0}_{-1.5}^{+1.7}-{11}_{-3}^{+4}$ depending on the assumed age of the field population (0.9–3.1 Gyr). We attribute the change in values to our use of kernel-phase interferometry, which enables us to resolve the peak of the semimajor axis distribution with significant sensitivity to low-mass companions. We confirm the previously seen trends of decreasing binary fraction with decreasing mass and a strong preference for tight and equal-mass systems in the field-age substellar regime; only ${0.9}_{-0.6}^{+1.1}$ % of systems are wider than 20 au and $\lt {1.0}_{-0.6}^{+1.4}$ % of systems have a mass ratio q < 0.6. We attribute this to turbulent fragmentation setting the initial conditions followed by a brief period of dynamical evolution, removing the widest and lowest-mass companions, before the birth cluster dissolves. Brown dwarfs L dwarfs T dwarfs Direct detection interferometry Direct imaging Hubble Space Telescope Astronomy Adam L. Kraus verfasserin aut In The Astronomical Journal IOP Publishing, 2022 165(2023), 3, p 130 (DE-627)312175647 (DE-600)2003104-X 15383881 nnns volume:165 year:2023 number:3, p 130 https://doi.org/10.3847/1538-3881/aca475 kostenfrei https://doaj.org/article/9bffad89f1b440cda889d9dad8a81274 kostenfrei https://doi.org/10.3847/1538-3881/aca475 kostenfrei https://doaj.org/toc/1538-3881 Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2006 GBV_ILN_2014 GBV_ILN_2088 GBV_ILN_2110 GBV_ILN_2129 GBV_ILN_2522 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 165 2023 3, p 130
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callnumber-first	Q - Science
author	Samuel M. Factor
spellingShingle	Samuel M. Factor misc QB1-991 misc Brown dwarfs misc L dwarfs misc T dwarfs misc Direct detection interferometry misc Direct imaging misc Hubble Space Telescope misc Astronomy NICMOS Kernel-phase Interferometry. II. Demographics of Nearby Brown Dwarfs
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topic_title	QB1-991 NICMOS Kernel-phase Interferometry. II. Demographics of Nearby Brown Dwarfs Brown dwarfs L dwarfs T dwarfs Direct detection interferometry Direct imaging Hubble Space Telescope
topic	misc QB1-991 misc Brown dwarfs misc L dwarfs misc T dwarfs misc Direct detection interferometry misc Direct imaging misc Hubble Space Telescope misc Astronomy
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title	NICMOS Kernel-phase Interferometry. II. Demographics of Nearby Brown Dwarfs
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title_sort	nicmos kernel-phase interferometry. ii. demographics of nearby brown dwarfs
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title_auth	NICMOS Kernel-phase Interferometry. II. Demographics of Nearby Brown Dwarfs
abstract	Star formation theories have struggled to reproduce binary brown dwarf population demographics (e.g., frequency, separation, and mass ratio). Kernel-phase interferometry is sensitive to companions at separations inaccessible to classical imaging, enabling tests of these theories at new physical scales below the hydrogen burning limit. We analyze the detections and sensitivity limits from our previous kernel-phase analysis of archival HST/NICMOS surveys of field brown dwarfs. After estimating physical properties of the 105 late-M to T dwarfs using Gaia distances and evolutionary models, we use a Bayesian framework to compare these results to a model companion population defined by log-normal separation and power-law mass-ratio distributions. When correcting for Malmquist bias, we find a companion fraction of $F={0.11}_{-0.03}^{+0.04}$ and a separation distribution centered at $\rho ={2.2}_{-1.0}^{+1.2}$ au, smaller and tighter than seen in previous studies. We also find a mass-ratio power-law index that strongly favors equal-mass systems: $\gamma ={4.0}_{-1.5}^{+1.7}-{11}_{-3}^{+4}$ depending on the assumed age of the field population (0.9–3.1 Gyr). We attribute the change in values to our use of kernel-phase interferometry, which enables us to resolve the peak of the semimajor axis distribution with significant sensitivity to low-mass companions. We confirm the previously seen trends of decreasing binary fraction with decreasing mass and a strong preference for tight and equal-mass systems in the field-age substellar regime; only ${0.9}_{-0.6}^{+1.1}$ % of systems are wider than 20 au and $\lt {1.0}_{-0.6}^{+1.4}$ % of systems have a mass ratio q < 0.6. We attribute this to turbulent fragmentation setting the initial conditions followed by a brief period of dynamical evolution, removing the widest and lowest-mass companions, before the birth cluster dissolves.
abstractGer	Star formation theories have struggled to reproduce binary brown dwarf population demographics (e.g., frequency, separation, and mass ratio). Kernel-phase interferometry is sensitive to companions at separations inaccessible to classical imaging, enabling tests of these theories at new physical scales below the hydrogen burning limit. We analyze the detections and sensitivity limits from our previous kernel-phase analysis of archival HST/NICMOS surveys of field brown dwarfs. After estimating physical properties of the 105 late-M to T dwarfs using Gaia distances and evolutionary models, we use a Bayesian framework to compare these results to a model companion population defined by log-normal separation and power-law mass-ratio distributions. When correcting for Malmquist bias, we find a companion fraction of $F={0.11}_{-0.03}^{+0.04}$ and a separation distribution centered at $\rho ={2.2}_{-1.0}^{+1.2}$ au, smaller and tighter than seen in previous studies. We also find a mass-ratio power-law index that strongly favors equal-mass systems: $\gamma ={4.0}_{-1.5}^{+1.7}-{11}_{-3}^{+4}$ depending on the assumed age of the field population (0.9–3.1 Gyr). We attribute the change in values to our use of kernel-phase interferometry, which enables us to resolve the peak of the semimajor axis distribution with significant sensitivity to low-mass companions. We confirm the previously seen trends of decreasing binary fraction with decreasing mass and a strong preference for tight and equal-mass systems in the field-age substellar regime; only ${0.9}_{-0.6}^{+1.1}$ % of systems are wider than 20 au and $\lt {1.0}_{-0.6}^{+1.4}$ % of systems have a mass ratio q < 0.6. We attribute this to turbulent fragmentation setting the initial conditions followed by a brief period of dynamical evolution, removing the widest and lowest-mass companions, before the birth cluster dissolves.
abstract_unstemmed	Star formation theories have struggled to reproduce binary brown dwarf population demographics (e.g., frequency, separation, and mass ratio). Kernel-phase interferometry is sensitive to companions at separations inaccessible to classical imaging, enabling tests of these theories at new physical scales below the hydrogen burning limit. We analyze the detections and sensitivity limits from our previous kernel-phase analysis of archival HST/NICMOS surveys of field brown dwarfs. After estimating physical properties of the 105 late-M to T dwarfs using Gaia distances and evolutionary models, we use a Bayesian framework to compare these results to a model companion population defined by log-normal separation and power-law mass-ratio distributions. When correcting for Malmquist bias, we find a companion fraction of $F={0.11}_{-0.03}^{+0.04}$ and a separation distribution centered at $\rho ={2.2}_{-1.0}^{+1.2}$ au, smaller and tighter than seen in previous studies. We also find a mass-ratio power-law index that strongly favors equal-mass systems: $\gamma ={4.0}_{-1.5}^{+1.7}-{11}_{-3}^{+4}$ depending on the assumed age of the field population (0.9–3.1 Gyr). We attribute the change in values to our use of kernel-phase interferometry, which enables us to resolve the peak of the semimajor axis distribution with significant sensitivity to low-mass companions. We confirm the previously seen trends of decreasing binary fraction with decreasing mass and a strong preference for tight and equal-mass systems in the field-age substellar regime; only ${0.9}_{-0.6}^{+1.1}$ % of systems are wider than 20 au and $\lt {1.0}_{-0.6}^{+1.4}$ % of systems have a mass ratio q < 0.6. We attribute this to turbulent fragmentation setting the initial conditions followed by a brief period of dynamical evolution, removing the widest and lowest-mass companions, before the birth cluster dissolves.
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container_issue	3, p 130
title_short	NICMOS Kernel-phase Interferometry. II. Demographics of Nearby Brown Dwarfs
url	https://doi.org/10.3847/1538-3881/aca475 https://doaj.org/article/9bffad89f1b440cda889d9dad8a81274 https://doaj.org/toc/1538-3881
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up_date	2024-07-03T21:37:08.830Z
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We also find a mass-ratio power-law index that strongly favors equal-mass systems: $\gamma ={4.0}_{-1.5}^{+1.7}-{11}_{-3}^{+4}$ depending on the assumed age of the field population (0.9–3.1 Gyr). We attribute the change in values to our use of kernel-phase interferometry, which enables us to resolve the peak of the semimajor axis distribution with significant sensitivity to low-mass companions. We confirm the previously seen trends of decreasing binary fraction with decreasing mass and a strong preference for tight and equal-mass systems in the field-age substellar regime; only ${0.9}_{-0.6}^{+1.1}$ % of systems are wider than 20 au and $\lt {1.0}_{-0.6}^{+1.4}$ % of systems have a mass ratio q < 0.6. 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