X-ray view of IC 348 in the light of an updated cluster census

Stelzer, B.; Preibisch, Thomas; Alexander, Frauke; Mucciarelli, P.; Flaccomio, E.; Micela, G.; Sciortino, S.

doi:10.1051/0004-6361/201118118

Cited by 36 publications

(69 citation statements)

References 55 publications

(91 reference statements)

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“…As Figure 1 demonstrates, such a trend of decreasing ( ) L L log X bol with M subtype is also apparent for the younger pre-MS M stars in the Taurus molecular clouds (median age ∼0.5 Myr; Grosso et al 2007) and for M stars in the young cluster IC 348 (age ∼3 Myr; Stelzer et al 2012). The decline of ( ) L L log X bol with decreasing M star effective temperature appears to be somewhat steeper in the TWA than in Taurus, and is similar to IC 348 in the range M0-M5.…”

Section: Trends In X-ray Luminosity and Disk Fractionmentioning

confidence: 74%

M Stars in the Tw Hya Association: Stellar X-Rays and Disk Dissipation

Kastner¹,

Principe²,

Punzi³

et al. 2016

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To investigate the potential connection between the intense X-ray emission from young low-mass stars and the lifetimes of their circumstellar planet-forming disks, we have compiled the X-ray luminosities (L X ) of M stars in the ∼8 Myr old TW Hya Association (TWA) for which X-ray data are presently available. Our investigation includes analysis of archival Chandra data for the TWA binary systems TWA 8, 9, and 13. Although our study suffers from poor statistics for stars later than M3, we find a trend of decreasing L L X bol with decreasing T eff for TWA M stars, wherein the earliest-typeand then ( ) L L log X bol decreases, and its distribution broadens, for types M4 and later. The fraction of TWA stars that display evidence for residual primordial disk material also sharply increases in this same (mid-M) spectral type regime. This apparent anticorrelation between the relative X-ray luminosities of low-mass TWA stars and the longevities of their circumstellar disks suggests that primordial disks orbiting early-type M stars in the TWA have dispersed rapidly as a consequence of their persistent large X-ray fluxes. Conversely, the disks orbiting the very lowest-mass pre-MS stars and pre-MS brown dwarfs in the Association may have survived because their X-ray luminosities and, hence, disk photoevaporation rates are very low to begin with, and then further decline relatively early in their pre-MS evolution.

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Section: Trends In X-ray Luminosity and Disk Fractionmentioning

confidence: 74%

M Stars in the Tw Hya Association: Stellar X-Rays and Disk Dissipation

Kastner¹,

Principe²,

Punzi³

et al. 2016

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“…Although in the near-IR, the triangular shape of the H-band caused by water absorption, with a peak redwards of that of field dwarfs (Luhman & Rieke 1999;Lucas et al 2001;McGovern et al 2004), is one of the youth indicators, at low signal-to-noise particular combinations of extinction and spectral type make the numerical fitting converge for both young and field dwarfs. We have also crossed-matched our candidates with the new reduction of deep X-ray observations of IC 348 (Stelzer et al 2012) but none of our candidates has been detected, though only 2 of the previously known brown dwarfs were identified. Given the depth of our spectroscopic survey, the sources of contamination are field dwarfs in the foreground and background of the cluster, as well as background giants.…”

Section: Membershipmentioning

confidence: 92%

“…The dashed line represents the field observed with WIRCam, the dash-dot line the X-ray observations analysed in Stelzer et al (2012), and the solid line delineates the area for which there is a complete census of the cluster for masses ≥30 M Jup (Luhman et al 2003b). members of the cluster.…”

Section: Colour−colour and Colour−magnitude Diagramsmentioning

confidence: 99%

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Spectroscopy of brown dwarf candidates in IC 348 and the determination of its substellar IMF down to planetary masses

Oliveira

Moraux

Bouvier

et al. 2013

A&A

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Context. Brown dwarfs represent a sizable fraction of the stellar content of our Galaxy and populate the transition between the stellar and planetary mass regime. There is, however, no agreement on the processes responsible for their formation. Aims. We have conducted a large survey of the young, nearby cluster IC 348, to uncover its low-mass brown dwarf population and have studied the cluster properties in the substellar regime. Methods. Deep optical and near-IR images taken with MegaCam and WIRCam at the Canada-France-Hawaii Telescope (CFHT) were used to select photometric candidate members. A spectroscopic follow-up of a large fraction of the candidates was conducted to assess their youth and membership. Results. We confirmed spectroscopically 16 new members of the IC 348 cluster, including 13 brown dwarfs, contributing significantly to the substellar census of the cluster, where only 30 brown dwarfs were previously known. Five of the new members have a L0 spectral type, the latest-type objects found to date in this cluster. At 3 Myr, evolutionary models estimate these brown dwarfs to have a mass of ∼13 M Jup . Combining the new members with previous census of the cluster, we constructed the initial mass function (IMF) complete down to 13 M Jup . Conclusions. The IMF of IC 348 is well fitted by a log-normal function and we do not see evidence for variations of the mass function down to planetary masses when compared to other young clusters.

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“…A general description of the resulting X-ray properties and an investigation of relations to the basic stellar parameters is given in Stelzer et al (2012). …”

Section: Chandra X-ray Observationsmentioning

confidence: 99%

X-ray activity and rotation of the young stars in IC 348

Alexander

Preibisch

2012

A&A

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Context. The physical origin of the strong magnetic activity in T Tauri stars and its relation to stellar rotation is not yet wellunderstood. Aims. We investigate the relation between the X-ray activity, rotation, and Rossby number for a sample of young stars in the ≈3 Myr old cluster IC 348. Methods. We use the data of four Chandra observations of IC 348 to derive the X-ray luminosities of the young stars. Basic stellar parameters and rotation rates are collected from the literature. This results in a sample of 82 X-ray detected stars with known rotation periods. We determine the Rossby numbers (i.e. the ratio of rotation period to convective turnover time) of 76 of these stars from stellar structure-and evolution-models for pre-main sequence stars.Results. The young stars in IC 348 show no correlation between X-ray activity and rotation period. For the Rossby numbers, nearly all IC 348 stars are in the saturated regime of the activity-rotation relation defined by main-sequence stars. Searching for possible super-saturation effects, we find a marginal (but statistically in-significant) trend that the stars with the smallest Rossby numbers have slightly lower X-ray activity levels. There are no significant differences in the X-ray activity level for stars of different spectral types and no relation between spectral type and Rossby number is seen. In addition, for stars belonging to different IR-classes, no significant differences are present for the X-ray activity level as well as for their Rossby numbers. We compare the dispersion in the fractional X-ray luminosities of the stars in the saturated rotation regime in IC 348 to that seen in younger and older stellar populations. The scatter seen in the ≈3 Myr old IC 348 [σ log (L X /L bol ) = 0.43] is considerably smaller than for the ≈1 Myr old Orion nebula cluster [σ log(L X /L bol ) = 0.63], but, at the same time, considerably larger than the dispersion seen in the ≈30 Myr old cluster NGC 2547 [σ log(L X /L bol ) = 0.24] and in main-sequence stars. Conclusions. The results of our X-ray analysis of IC 348 show that neither the rotation rates nor the presence/absence of circumstellar disks are of fundamental importance for determining the level of X-ray activity in TTS. Our results suggest that the scatter in the X-ray activity levels for the rapidly rotating members of young clusters decreases with the age of the stellar population. We interpret this as a signature of the changing interior structure of pre-main sequence stars and the consequent changes in the dynamo mechanisms that are responsible for the magnetic field generation.

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X-ray view of IC 348 in the light of an updated cluster census

Cited by 36 publications

References 55 publications

M Stars in the Tw Hya Association: Stellar X-Rays and Disk Dissipation

M Stars in the Tw Hya Association: Stellar X-Rays and Disk Dissipation

Spectroscopy of brown dwarf candidates in IC 348 and the determination of its substellar IMF down to planetary masses

X-ray activity and rotation of the young stars in IC 348

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