Figure 4 - uploaded by Patricia Luppe
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Same as Fig. 1, but with the 15 min IRAM detection limits overplotted. The light green curve represents the IRAM 1 mm band and the dark green curve shows the IRAM 2 mm band.
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Debris discs are second generation dusty discs formed by collisions of planetesimals. Many debris discs have been found and resolved around hot and solar-type stars. However, only a handful have been discovered around M-stars, and the reasons for their paucity remain unclear. Here we check whether the sensitivity and wavelength coverage of present-...
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Citations
... Infra-Red emission from M dwarfs has been investigated in multiple studies. Extra flux in the IR range characterized the circumstellar dust which mark certain stages in the life of a planetary system (protoplanetary disc, and final stage is a debris disc, Luppe et al. (2020). Sgro & Song (2021) used Gaia DR2 and ALLWISE W3 and W4 passbands to search for M dwarfs with IR-excess, within 100 pc. ...
In this paper we report about 100 new M dwarfs, confirmed in the DFBS database. The DFBS is the digitized version of the First Byurakan Survey (FBS, or Markarian survey). FBS plates have been used to search and study faint Late-Type Stars (LTS). The confirmations is based on Gaia DR3 BP/RP spectral database. In previous studies of the DFBS plates, these objects were presented as LTS candidates. TESS phased light curves for some of them shows flares. In SEDs of these objects the infrared excess is clearly visible.
... Though M dwarfs make up approximately 80% of nearby stars (Reylé et al. 2021), few M dwarf debris disks have been identified, and fewer have been studied in detail (e.g., Avenhaus et al. 2012;Luppe et al. 2020;Ren et al. 2021;Cronin-Coltsmann et al. 2023). Of the 10 known M dwarf debris disk systems within 100 pc, only five have had their disks definitively spatially resolved (Cronin-Coltsmann et al. 2023), and only four have been detected in scattered light. ...
... 12 The small sample of M dwarf debris disks available for study precludes assessment of how the debris disks of the low-mass majority of stars, and thus their planetary systems, differ from those of more massive stars. While numerous studies have proposed mechanisms that might lead to M dwarf debris disks being intrinsically less common than those of higher-mass stars (e.g., Lestrade et al. 2011), recent results suggest that they are equally abundant but are often simply too faint to detect (Luppe et al. 2020;Cronin-Coltsmann et al. 2023). Moreover, simply detecting an M dwarf debris disk is not sufficient for accessing the wealth of information that debris disks can provide. ...
... With many important scatteredlight spectral features occurring at these wavelengths (e.g., the 3 μm water-ice feature; Kim et al. 2019), detections here are particularly powerful for diagnosing debris disk composition. Combined with the utility of ALMA for providing thermal detections of these objects (Luppe et al. 2020;Cronin-Coltsmann et al. 2023), JWST detections in scattered light may provide a compelling new avenue for understanding the planetary systems of M dwarfs. Lawson et al. (2023) demonstrated the efficacy of NIRCam coronagraphy for studying M dwarf debris disks at 3-5 μm in application to the debris disk of AU Mic. ...
Observations of debris disks offer important insights into the formation and evolution of planetary systems. Though M dwarfs make up approximately 80% of nearby stars, very few M dwarf debris disks have been studied in detail—making it unclear how or if the information gleaned from studying debris disks around more massive stars extends to the more abundant M dwarf systems. We report the first scattered-light detection of the debris disk around the M4 star Fomalhaut C using JWST's Near Infrared Camera (NIRCam; 3.6 and 4.4 μ m). This result adds to the prior sample of only four M dwarf debris disks with detections in scattered light and marks the latest spectral type and oldest star among them. The size and orientation of the disk in these data are generally consistent with the prior Atacama Large Millimeter/submillimeter Array submillimeter detection. Though no companions are identified, these data provide strong constraints on their presence—with sensitivity sufficient to recover sub-Saturn mass objects in the vicinity of the disk. This result illustrates the unique capability of JWST to uncover elusive M dwarf debris disks in scattered light and lays the groundwork for deeper studies of such objects in the 2–5 μ m regime.
... The Atacama Large Millimetre Array (ALMA) is the best-suited contemporary telescope to fulfill these requirements. Luppe et al. ( 2020 ) investigate the capability of ALMA to detect a population of M-dwarf discs around the DEBRIS sample of M-stars, assuming that those discs have the same properties as the DEBRIS FGK-type systems. They conclude that for 15 min of observation at Band 7, there would be a 4 per cent-16 per cent detection rate if all the discs were unresolved and a detection rate of 1 per cent-6 per cent if some discs are large or close enough to be resolved. ...
... We now compare to the Luppe et al. ( 2020 ) predictions for an ALMA surv e y of DEBRIS-like M-dwarf discs. Our sample has been observed for approximately 15 min per star with ALMA Band 7, and the observations were designed to reduce the likelihood that discs would be resolved. ...
... It is unlikely that any discs would be larger than the maximum reco v erable scales of our observations, but as evidenced by GSC 07396 −00759 discs could still have been resolved, reducing the flux per beam. Without correcting for resolution Luppe et al. ( 2020 ) predict 15 min of observation at Band 7 of the Herschel DEBRIS sample of M-dwarfs scaled as DEBRIS-like discs to attain a detection rate of 4.3 ± 0.9 per cent to 15.8 ± 0.5 per cent, entirely consistent with our observations. If the DEBRIS sample and the BPMG stellar samples are broadly similar, this would imply that M-dwarf discs are o v erall similar to earlier type stars' discs in terms of radius, total surface area, temperature and fractional luminosity, when scaled by stellar mass and luminosity. ...
Previous surveys in the far-infrared have found very few, if any, M-dwarf debris discs among their samples. It has been questioned whether M-dwarf discs are simply less common than earlier types, or whether the low detection rate derives from the wavelengths and sensitivities available to those studies. The highly sensitive, long wavelength Atacama Large Millimetre/submillimetre Array can shed light on the problem. This paper presents a survey of M-dwarf stars in the young and nearby Beta Pictoris Moving Group with ALMA at Band 7 (880 μm). From the observational sample we detect two new sub-mm excesses that likely constitute unresolved debris discs around GJ 2006 A and AT Mic A and model distributions of the disc fractional luminosities and temperatures. From the science sample of 36 M-dwarfs including AU Mic we find a disc detection rate of 4/36 or 11.1% that rises to 23.1% when adjusted for completeness. We conclude that this detection rate is consistent with the detection rate of discs around G and K type stars and that the disc properties are also likely consistent with earlier type stars. We additionally conclude that M-dwarf stars are not less likely to host debris discs, but instead their detection requires longer wavelength and higher sensitivity observations than have previously been employed.
... Cotten & Song (2016) reported on about near 500 IR-excess stars. Extra flux in the IR range characterised the circumstellar dust which mark certain stages in the life of a planetary system (protoplanetary disc, and final stage is a debris disc, Luppe et al. (2020)). Sgro & Song (2021) used Gaia DR2 and ALLWISE W3 and W4 passbands to search for M dwarfs with IR-excess, within 100 pc. ...
In order to gain more information on the 236 M dwarfs identified in the First Byurakan Survey (FBS) low-resolution (lr) spectroscopic database, Gaia EDR3 high-accuracy astrometric and photometric data and Transiting Exoplanet Survey Satellite (TESS) data are used to characterize these M dwarfs and their possible multiplicity. Among the sample of 236 relatively bright (7.3 < K s < 14.4) M dwarfs, 176 are new discoveries. The Gaia EDR3 G broad-band magnitudes are in the range 11.3 < G < 17.1. New distance information based on the EDR3 parallaxes are used to estimate the G-band absolute magnitudes. 9 FBS M dwarfs out of 176 newly discovered lie within 25 pc of the Sun. The FBS 0909-082 is the most distant (r= 780 pc) M dwarf of the analyzed sample, with a G-band absolute magnitude , and T eff = 3844 K.; it can be classified as M1 – M2 subtype dwarf. The nearest is FBS 0250+167, a M7 subtype dwarf located at 3.83 pc from the Sun with a very high proper motion (5.13 arcsec/yr). The TESS estimated masses lie in the range and T eff in the range 4000 K < T eff < 2790 K. We analyze color-color and color-absolute magnitude diagram (CaMD) diagrams for the M dwarfs. Results suggest that 27 FBS M dwarfs are double or multiple systems. The observed spectral energy distribution (SED) for some of the M dwarfs can be used to classify potential Infra-Red (IR) excess. Using TESS light curves, flares are detected for some FBS M dwarfs. Finally, for early and late sub-classes of the M dwarfs the detection range for survey is estimated for the first time.
... One difficulty in the protoplanetary disk -exocometary belt observational comparison is that most of the protoplanetary disks in nearby star-forming regions surround lowmass stars, whereas the majority of detectable exocometary belts orbit around A-F stars, likely due to current lack of sensitivity to belts around later-type stars, particularly M dwarfs (Luppe et al. 2020). In general, the presence of evolved Class III disks in young star forming regions, with masses consistent with young exocometary belts, suggests that exocomets can form early on, within the first ∼2 Myr (Lovell et al. 2021). ...
In this chapter we review our knowledge of our galaxy's cometary population outside our Oort Cloud - exocomets and Interstellar Objects (ISOs). We start with a brief overview of planetary system formation, viewed as a general process around stars. We then take a more detailed look at the creation and structure of exocometary belts, as revealed by the unprecedented combination of theoretical and observational advances in recent years. The existence and characteristics of individual exocomets orbiting other stars is summarized, before looking at the mechanisms by which they may be ejected into interstellar space. The discovery of the first two ISOs is then described, along with the surprising differences in their observed characteristics. We end by looking ahead to what advances may take place in the next decade.
... Theissen & West (2014) found evidence for warm dust around a sample of M dwarfs (see their Table 5 for the minimum orbital distance of the dust). Currently, there is no evidence of even a Kuiper Belt equivalent in TRAPPIST-1 (Marino et al. 2020) although in general, cold debris disks are found around a similar fraction of M dwarfs as higher-mass stars (Lestrade et al. 2006;Luppe et al. 2020). ...
Exoplanets orbiting in the habitable zone around M dwarf stars have been prime targets in the search for life due to the long lifetimes of the host star, the prominence of such stars in the galaxy, and the apparent excess of terrestrial planets found around M dwarfs. However, the heightened stellar activity of M dwarfs and the often tidally locked planets in these systems have raised questions about the habitability of these planets. In this Letter we examine another significant challenge that may exist: these systems seem to lack the architecture necessary to deliver asteroids to the habitable terrestrial planets, and asteroid impacts may play a crucial role in the origin of life. The most widely accepted mechanism for producing a stable asteroid belt and the late-stage delivery of asteroids after gas disk dissipation requires a giant planet exterior to the snow-line radius. We show that none of the observed systems with planets in the habitable zone of their star also contain a giant planet and therefore are unlikely to have stable asteroid belts. We consider the locations of observed giant planets relative to the snow-line radius as a function of stellar mass and find that there is a population of giant planets outside of the snow-line radius around M dwarfs. Therefore, asteroid belt formation around M dwarfs is generally possible. However, we find that multiplanetary system architectures around M dwarfs can be quite different from those around more massive stars.
... Theissen & West (2014) found evidence for warm dust around a sample of M-dwarfs (see their table 5 for the minimum orbital distance of the dust). Currently, there is no evidence of even a Kuiper belt equivalent in TRAPPIST-1 (Marino et al. 2020) although in general, cold debris disks are found around a similar fraction of M-dwarfs as higher mass stars (Lestrade et al. 2006;Luppe et al. 2020). ...
Exoplanets orbiting in the habitable zone around M-dwarf stars have been prime targets in the search for life due to the long lifetimes of the host star, the prominence of such stars in the galaxy, and the apparent excess of terrestrial planets found around M-dwarfs. However, the heightened stellar activity of M-dwarfs and the often tidally locked planets in these systems have raised questions about the habitability of these planets. In this letter we examine another significant challenge that may exist: these systems seem to lack the architecture necessary to deliver asteroids to the habitable terrestrial planets, and asteroid impacts may play a crucial role in the origin of life. The most widely accepted mechanism for producing a stable asteroid belt and the late stage delivery of asteroids after gas disk dissipation requires a giant planet exterior to the snow line radius. We show that none of the observed systems with planets in the habitable zone of their star also contain a giant planet and therefore are unlikely to have stable asteroid belts. We consider the locations of observed giant planets relative to the snow line radius as a function of stellar mass and find that there is a population of giant planets outside of the snow line radius around M-dwarfs. Therefore, asteroid belt formation around M-dwarfs is generally possible. However, we find that multi-planetary system architectures around M-dwarfs can be quite different from those around more massive stars.
... Plavchan et al. 2005Plavchan et al. , 2009Gautier et al. MNRAS 512, 4752-4764 (2022) 2007 ; Heng & Malik 2013 ;Binks & Jeffries 2017 ;Luppe et al. 2020 ) as to whether so few M-dwarf discs have been detected because they represent a fundamentally rarer and/or lower mass population to those of earlier type hosts, or whether the low luminosity of the host M-dwarfs, resulting in low disc fluxes and temperatures, hinders a similar population from being detectable. Later type stars have a measured increase in planet occurrence rate (e.g. ...
We present new ALMA Band 7 observations of the edge-on debris disc around the M1V star GSC 07396-00759. At ∼20 Myr old and in the β Pictoris Moving Group along with AU Mic, GSC 07396-00759 joins it in the handful of low mass M-dwarf discs to be resolved in the sub-mm. With previous VLT/SPHERE scattered light observations we present a multi-wavelength view of the dust distribution within the system under the effects of stellar wind forces. We find the mm dust grains to be well described by a Gaussian torus at 70 au with a FWHM of 48 au and we do not detect the presence of CO in the system. Our ALMA model radius is significantly smaller than the radius derived from polarimetric scattered light observations, implying complex behaviour in the scattering phase function. The brightness asymmetry in the disc observed in scattered light is not recovered in the ALMA observations, implying that the physical mechanism only affects smaller grain sizes. High resolution follow-up observations of the system would allow investigation into its unique dust features as well as provide a true coeval comparison for its smaller sibling AU Mic, singularly well observed amongst M-dwarfs systems.
... There is thus an open question (e.g. Plavchan et al. 2005Plavchan et al. , 2009Gautier et al. 2007;Heng & Malik 2013;Binks & Jeffries 2017;Luppe et al. 2020) as to whether so few M-dwarf discs have been detected because they represent a fundamentally rarer and/or lower mass population to those of earlier type hosts, or whether the low luminosity of the host M-dwarfs, resulting in low disc fluxes and temperatures, hinders a similar population from being detectable. Later type stars have a measured increase in planet occurrence rate (e.g. ...
We present new ALMA Band 7 observations of the edge-on debris disc around the M1V star GSC 07396-00759. At ~20 Myr old and in the beta Pictoris Moving Group along with AU Mic, GSC 07396-00759 joins it in the handful of low mass M-dwarf discs to be resolved in the sub-mm. With previous VLT/SPHERE scattered light observations we present a multi-wavelength view of the dust distribution within the system under the effects of stellar wind forces. We find the mm dust grains to be well described by a Gaussian torus at 70 au with a FWHM of 48 au and we do not detect the presence of CO in the system. Our ALMA model radius is significantly smaller than the radius derived from polarimetric scattered light observations, implying complex behaviour in the scattering phase function. The brightness asymmetry in the disc observed in scattered light is not recovered in the ALMA observations, implying that the physical mechanism only affects smaller grain sizes. High resolution follow-up observations of the system would allow investigation into its unique dust features as well as provide a true coeval comparison for its smaller sibling AU Mic, singularly well observed amongst M-dwarfs systems.
... The observed occurrence rate as function of stellar mass for debris disks and structured disks is indeed similar (van der Marel & Mulders 2021). One caveat in the comparison of occurrence rates is that debris disks around M stars are particularly scarce down to existing detection limits (Luppe et al. 2020). We suggest that there may be inherently fewer debris disks around M stars due to their possible lack of formation; in addition, the effects of rapid collisional evolution and stellar winds to deplete and cut off the dust size distribution render those that do exist particularly difficult to detect (Plavchan et al. 2005). ...
... As we continue to develop a better and more thorough understanding of disk evolution, we pose some new questions: How low can Class III mm-dust masses be, and do they display the same distribution (across 3 orders of magnitude) as Class II disks? Are they underrepresented due to sensitivity as proposed by Luppe et al. (2020) or are most M-star protoplanetary disks so significantly radial drift dominated that these result in near diskless stars? At what moment does the UV-switch take place, overtaking the accretion rate and rapidly clearing out the gas? ...
The connection between the nature of a protoplanetary disk and that of a debris disk is not well understood. Dust evolution, planet formation, and disk dissipation likely play a role in the processes involved. We aim to reconcile both manifestations of dusty circumstellar disks through a study of optically thin Class III disks and how they correlate to younger and older disks. In this work, we collect literature and Atacama Large Millimeter/submillimeter Array archival millimeter fluxes for 85 disks (8%) of all Class III disks across nearby star-forming regions. We derive millimeter-dust masses M dust and compare these with Class II and debris disk samples in the context of excess infrared luminosity, accretion rate, and age. The mean M dust of Class III disks is 0.29 ± 0.19 M ⊕ . We propose a new evolutionary scenario wherein radial drift is very efficient for nonstructured disks during the Class II phase resulting in a rapid M dust decrease. In addition, we find possible evidence for long infrared protoplanetary disk timescales, ∼8 Myr, consistent with overall slow disk evolution. In structured disks, the presence of dust traps allows for the formation of planetesimal belts at large radii, such as those observed in debris disks. We propose therefore that the planetesimal belts in debris disks are the result of dust traps in structured disks, whereas protoplanetary disks without dust traps decrease in dust mass through radial drift and are therefore undetectable as debris disks after the gas dissipation. These results provide a hypothesis for a novel view of disk evolution.
