Characterisation of AstraLux binaries

Characterisation of close visual binaries from the AstraLux Large M Dwarf Survey1

Abstract

We present VLT/SINFONI spectra of seven close visual pairs in M dwarf binary/triple systems, discovered or observed by the AstraLux M dwarf survey. We determine the spectral types to within subclasses from comparison to template spectra and the strength of -band water absorption, and derive effective temperatures. The results are compared to optical spectral types of the unresolved binary/multiple systems, and we confirm that our photometric method to derive spectral types in the AstraLux M dwarf survey is accurate. We look for signs of youth such as chromospheric activity and low surface gravity, and find an age in the range  Gyr for the GJ 852 system. Strong Li absorption is detected in optical spectra of the triple system J024902 obtained with FEROS at the ESO-MPG 2.2 m telescope. The equivalent width of the absorption suggests an age consistent with the Pic moving group. However, further observations are needed to establish group membership. Ongoing orbital monitoring will provide dynamical masses and thus calibration of evolutionary models for low mass stars.

keywords:
stars: low-mass – stars: fundamental parameters – stars: pre-main-sequence – binaries: visual
24

1 Introduction

M dwarfs in multiple systems can provide valuable insight into the structure, formation and evolution of very-low mass stars and brown dwarfs, through their multiplicity characteristics as well as their physical and orbital properties (e.g., Burgasser et al., 2007; Goodwin et al., 2007; Janson et al., 2007; Duchêne & Kraus, 2013). Despite being the most common stars in our neighbourhood, fundamental physical characteristics such as mass, radius, luminosity, and relations between these properties, are not as well constrained for mid- to late-M type dwarfs as for solar-type and intermediate mass stars. Detailed studies of orbital elements of individual low mass binaries, and dynamical masses, are needed for empirical calibration of models for low-mass stars, and significant effort has therefore been made in recent years to better characterise in particular ultra-cool dwarfs (e.g. Bouy et al., 2008; Bonnefoy et al., 2009; Konopacky et al., 2010; Dupuy et al., 2010; Schlieder et al., 2014; Zhou et al., 2014). In addition, the recent discoveries and dedicated surveys for M dwarf planets require accurate stellar physical properties in order to derive reliable planetary parameters, furthering the interest for characterising M dwarfs (e.g., Johnson et al., 2012; Mann et al., 2012, 2013; Mann, Gaidos & Ansdell, 2013; Muirhead et al., 2012, 2014; Dressing & Charbonneau, 2013; Newton et al., 2014, 2015; Gaidos et al., 2014; Alonso-Floriano et al., 2015; Bowler et al., 2015).

Atmospheric and evolutionary models are particularly poorly constrained for young ( Myr) M dwarfs, of which only a handful of binaries have measured dynamical masses (see, e.g., Close et al., 2005; Bonnefoy et al., 2009). In order to better constrain multiplicity properties and identify young binaries suitable for dynamical mass measurements, we carried out the AstraLux large M dwarf survey: a Lucky Imaging multiplicity survey of 761 young, nearby late-K and M dwarfs (Bergfors et al., 2010; Janson et al., 2012), supplemented by 286 mid- to late-M dwarfs in an extension of the survey (Janson et al., 2014a). From this survey we selected seven pairs in binary or triple systems for the spectroscopic observations presented in this paper, to better characterise the stars with respect to spectral types and youth. A large fraction of the AstraLux targets, including five of the binaries studied here, have recently been kinematically linked to young associations (Malo et al., 2013, 2014a; Rodriguez et al., 2013, Schlieder et al., in preparation). Observed properties such as spectral type, surface gravity and luminosity can be compared to evolutionary models of pre-main sequence stars to yield component mass and system age estimates for close binaries. Ongoing astrometric and radial velocity monitoring will provide a better understanding of these objects from well determined orbits and dynamical masses within a few years, which will then be compared to the results presented here.

This paper is organised as follows: After a short introduction in Section 1, Section 2 describes the target selection, observations and data reduction procedure. In Section 3, the individual component spectral types and effective temperatures are determined and compared to previous estimates. We also measure the equivalent widths of gravity sensitive features and compare to old field stars and to stars in young associations. We discuss our results and additional youth indicators in Section 4, and compare the observed and derived vs. of GJ 852 BC and J061610 to theoretical isochrones to infer individual masses and system ages. We end this report with a summary of our results and conclusions in Section 5.

2 Observations and data reduction

2.1 Target selection and observations

Seven nearby M dwarf binaries or close pairs in hierarchical triple systems were selected from the target list of the AstraLux M dwarf survey as good candidates for follow-up near-infrared spectroscopy and characterisation. These are listed in Table LABEL:observations. The selected targets had all been observed in at least two epochs and were confirmed as physically bound via common proper motion. They all had a projected separation of  AU and primaries with photometric spectral types M3.5 or later derived from AstraLux observations in SDSS and band. The stars in the AstraLux survey are suspected to be young, based on their coronal activity and low tangential velocity, and have spectroscopic distances of less than 52 pc from the Sun (Riaz, Gizis & Harvin, 2006). The GJ 852 BC system has a USNO parallax distance of only 10 pc (Harrington & Dahn, 1980).

The targets were observed in service mode with the adaptive optics fed Spectrograph for INtegral Field Observations in the Near Infrared (SINFONI, Bonnet et al., 2004) at the VLT Unit Telescope 4 (Yepun). SINFONI consists of the SPIFFI integral field spectrograph (Eisenhauer et al., 2003) together with the Multi-Application Curvature Adaptive Optics module (MACAO, Bonnet et al., 2003). We used the (m) and (m) gratings, with a resolving power of R2000 and 1500 respectively, and the target itself as a natural guide star. Pre-slit optics were selected depending on binary separation to provide a spaxel scale of , corresponding to a Field of View (FoV) of arcsec, for all the targets with angular separations (see Table LABEL:observations). For the wider couple, GJ 852 BC, the spaxel pre-optics were used, corresponding to a FoV of 8 arcsec. Each target was observed in a dither sequence with small offsets between eight science exposures, and three sky dither points at the beginning, middle and end of science acquisition. For each observation a telluric standard star of spectral type B or early A was observed at similar airmass. All observations were performed at airmass close to 1.0. Table LABEL:observations lists the observational details: which components were observed (GJ 852 BC, J053018 AB and J024902 BC are part of triple systems with a wider companion), their angular separation as measured by Bergfors et al. (2010); Janson et al. (2012), the date of observation, integration times and number of integrations, measured Signal-to-Noise ratio (S/N, see Sect. 3.1) and the spectral type of the telluric standard.

2MASS ID Comp.5 6 Obs. Date Exp. Time Exp. Time -band S/N -band S/N -band S/N Telluric Std
[″] Prim/Sec Prim/Sec Prim/Sec SpT
J02133021-4654505 A, B 0.138 2011-11-15  s  s 51/26 58/60 90/82 B9 V
J02490228-1029220 B, C 0.157 2010-12-01  s  s 20/20 34/34 39/33 B8 V
J04080543-2731349 A, B 0.221 2011-01-09  s  s 18/14 17/22 23/15 B3 V
J05301858-5358483 A, B 0.232 2011-11-16  s  s 92/90 73/61 95/69 B8 V
J06134539-2352077 A, B 0.145 2011-11-16  s  s 97/64 67/67 74/58 B8 V
J06161032-1320422 A, B 0.194 2010-12-01  s  s 43/22 26/15 22/9 B9 V
J22171899-0848122 B, C 0.970 2010-10-21  s  s 63/32 86/56 95/45 A0 V

7

See Bergfors et al. (2010); Janson et al. (2012) for component definitions and astrometric measurements.

Table 1: SINFONI observational details.

2.2 Data reduction

and band datacubes were built from a set of raw data and associated calibration frames using the SINFONI data reduction pipeline version 2.2.5 (Abuter et al., 2006). Some of the raw frames were affected by stripes on slitlet (the so called odd/even effect8) and by dark horizontal lines. These electronic artefacts were properly removed using custom scripts before providing the frames to the pipeline. The data reduction was checked by eye and a set of quality control parameters were compared to reference values9.

Though the binaries are successfully resolved by MACAO, cross contamination of their spectra is an issue that must be addressed. We used a custom spectral extraction tool to deblend the flux of the components, and consequently their spectra, slice by slice in each of the datacubes. The tool is a modified version of the algorithm presented in Bonnefoy et al. (2009). It first estimates the positions of the sources inside the FoV, which usually drift due to the atmospheric refraction10. We then applied on each slice a modified version of the Dumas et al. (2001) CLEAN algorithm to retrieve the individual flux of the sources. The algorithm requires the PSF at the time of the observation and for each cube wavelength. To provide that, we considered two different approaches. We first used a scaled version of the telluric standard star data cubes observed immediately after our targets (hereafter PSFstd). Alternatively, we built the PSF by duplicating the profile (hereafter PSFdup) of the brightest binary component (or of the component farthest from the FoV edges). We re-estimated the position of the sources, and re-built the PSF in case PSFdup was chosen, applying a second layer of CLEAN. For each input cube, an extracted cube for each binary component, and a residual map that enables to monitor the efficiency of the extraction process was produced. PSFdup provides a more accurate extraction. On the contrary, the PSF shape built following PSFstd is less appropriate, but the resulting spectra have slightly higher S/N in some cases. Since our spectral analysis is based mainly on the continuum shape (see Section 3.1), we used the PSFdup reduced spectra for our analysis.

The science target and telluric standard spectra were extracted using the same aperture sizes for target and standard star so as to minimise differential flux losses. Aperture sizes of 225 mas were considered optimal for obtaining high S/N for the small plate scale observations, and a 900 mas aperture was used for GJ 852 BC. For each set of observations, the strong Br-series absorption lines in and the Pa line in -band in our late-B – early-A telluric standard spectra were fitted with Voigt functions and subtracted from the standard star spectrum before it was divided by a blackbody function of corresponding temperature. The science spectrum was then divided by the resulting spectral response, containing only remaining instrumental and atmospheric features, to obtain the final spectrum.

3 Results

3.1 Spectral type and effective temperature

The strong atomic and molecular features and temperature sensitive continuum regions make -band the optimal choice for determining spectral types of cool stars in the near-infrared. As a first estimate, we performed a visual comparison of the -band spectral shapes to template SpeX spectra obtained from the IRTF Spectral Library (Cushing, Rayner & Vacca, 2005; Rayner, Cushing & Vacca, 2009). We also compared the strengths of some of the most prominent atomic and molecular absorption features in - and -band suitable for spectroscopic classification, such as Na, Ca, Al, Mg, Si, Fe, and CO and FeH band heads (Cushing, Rayner & Vacca, 2005), to the IRTF templates.

The S/N was measured in each wavelength band in small regions without prominent spectral features as suggested by Covey et al. (2010), and are listed in Table LABEL:observations. Note that these values are representative and vary over the spectral range. The low S/N of the J040805 and J061610 spectra makes it difficult to assign precise spectral types to these targets based on absorption feature strengths, and we estimated rough spectral types for these stars from the continuum shapes in the -band.

Figures 1–4 show our and band spectra plotted together with the SpeX templates. For this and following analysis, we used the spectra extracted using the PSFdup-method since it best preserves the individual spectral shapes. The -band spectra of J024902 and J040805 are of low S/N () and are omitted from Figure 1 as no atomic features could be confidently identified.

Figure 1: -band spectra. The SINFONI targets are shown in black, and IRTF templates in blue.

The initial estimate is complemented by a more quantitative spectral type analysis in which we calculated the -index defined by Rojas-Ayala et al. (2012):

(1)

The index is a modified version of the Covey et al. (2010) -index which takes into account the Mg I and Ti I atomic features that affect the measurements in bright spectra. It measures the temperature dependent strength of -band water absorption and is independent of gravity and metallicity for  K. We measured the median flux in each wavelength region in Eq. 1 and estimated errors with a Monte Carlo simulation. Random Gaussian noise based on the S/N was added to a set of 10 000 median flux measurements, from which the mean index was calculated with error bars corresponding to the standard deviation of the resulting distribution. The indices and corresponding spectral types are listed in Table LABEL:SpT, together with the spectral types derived from by Bergfors et al. (2010); Janson et al. (2012) and the visually estimated -band spectral types.

We derive the effective temperatures using the spectral type – effective temperature relations for  Myr old M dwarfs from Kraus & Hillenbrand (2007). The results are listed in Table LABEL:SpT and assume errors in directly corresponding to the estimated errors of the adopted spectral type.

Figure 2: Similar to Fig. 1 but for -band.
ID () SpT NIR SpT HO-K2 NIR SpT Adopted SpT
Photometry K-band comp. HO-K2 (K)
J021330 (A) M4.0 () M3.0M3.5 M3.5 () M3.5 ()
J021330 (B) M5.0 () M3.0M3.5 M3.5 () M3.5 ()
J024902 (B) M3.5 () M4.0 M4.0 () M4.0 ()
J024902 (C) M3.5 () M4.0M4.5 M4.0 () M4.0 ()
J040805 (A) M3.5 () M3.0M3.5 M1.0 (-) M3.5 ()
J040805 (B) M4.5 () M3.0M4.0 M3.5 () M4.0 ()
J053018 (A) M3.0 () M2.0M3.0 M1.5 () M2.0 ()
J053018 (B) M4.0 () M3.0 M3.5 () M3.5 ()
J061345 (A) M3.5 () M3.5 M3.5 () M3.5 ()
J061345 (B) M5.0 () M3.5M4.5 M4.0 () M4.0 ()
J061610 (A) M3.5 () M3.0M4.0 M4.0 () M3.5 ()
J061610 (B) M5.0 () M4.0M6.0 M7.0 () M5.0 ()
Gl 852 (B) M4.5 () M4.0M5.0 M5.0 () M4.5 ()
Gl 852 (C) M8.5 () M7.0M8.0 M7.5 () M7.5 ()

Table 2: Photometric and near-infrared spectral types, and inferred effective temperatures.
Figure 3: -band spectra for GJ 852 BC. The SINFONI targets are shown in black, and comparison IRTF templates in magenta.
Figure 4: Similar to Fig. 3 but for -band.

3.2 Comparison of near-infrared spectral types to AstraLux optical photometry

In order to derive approximate spectral types for the binary or multiple systems discovered in the AstraLux M dwarf survey and exclude background contaminants, each target was observed in SDSS - and -band and individual spectral types were derived from colours and the integrated spectral types, with estimated errors of spectral subtype (see Daemgen et al., 2009; Bergfors et al., 2010). Obtaining near-infrared spectral types allows us to better quantify the precision of the photometric spectral types, as derived for individual M dwarf binary components in Bergfors et al. (2010); Janson et al. (2012, 2014a), and identify potential biases in the method. We find that, with the exception of J021330 B, all near-infrared spectral types agree with the photometrically derived spectral types within the photometric subclass error, and in most cases to within 0.5 subclasses (see Table LABEL:SpT). This confirms that the photometric method used in the AstraLux large M dwarf survey in general provides accurate spectral types.

3.3 Comparison with integrated optical spectral types

FEROS observations and data reduction

For some of our targets spatially unresolved optical spectroscopy exists, obtained with the Fiberfed Extended Range Optical Spectrograph (FEROS, Kaufer et al., 1999) mounted to the ESO-MPG 2.2 m telescope at La Silla Observatory. J053018 and J061345 were observed within the ESO programmes 086.A-9014 and 089.A-9013 (Bergfors et al., in preparation), and J024902 within programme 088.A-9032 (Schlieder et al., in preparation). Additional FEROS spectra of J021330 were retrieved from the ESO archive (programme ID 091.C-0216, PI: Rodriguez). FEROS provides spectra covering across 39 orders at , using two optical fibres separated by . The targets were observed in ‘object+sky’ mode with one fibre on the star and the other on sky, and at airmass close to 1.0. Observational details are provided in Table LABEL:optSpT.

The data were reduced using the FEROS Data Reduction System (DRS) within the ESO-MIDAS package. The package follows standard spectroscopic reduction procedures which include flat-fielding, background subtraction, bad pixel correction, optimal order extraction, and wavelength calibration using ThAr lamp lines. The software also computes the barycentric velocity correction and re-bins and merges the orders to produce a continuous spectrum. Calibrations used during the reduction were acquired in daytime. For J024902, the RV standard GJ 1094 was observed on the previous night as an internal calibration check.

Optical spectral types

We determined integrated optical spectral types for these systems by comparing TiO and CaH band head strengths to M dwarf spectral templates from the Sloan Digital Sky Survey (Bochanski et al., 2007). Section 4.1.2 provides details on additional analysis performed for J024902.

An earlier optical spectral type of is found for the M4+M4 system J024902 compared to the photometric resolved optical spectral types, due to the inclusion of the early M primary in the FEROS fibre aperture (J024902 A, , see also Sect. 4.1.2). The optical spectral types are otherwise fully consistent with the AstraLux photometric spectral types. Our optical and near-infrared spectral types agree within errors, which is to be expected on average.

ID Obs. Date Optical SpT Exp. Time
[s]
J021330 2013-09-23 M4M5 4 600
J024902 2011-12-06 M2 1 2300
J053018 2010-11-25, 2012-08-22 M3M4 1 900, 1 900
J061345 2010-11-22, 2012-08-29 M4 1 900, 1 900

Table 3: FEROS observational details and optical spectral types.

3.4 Surface gravity and chromospheric activity

Age is one of the most difficult stellar parameters to determine. A combination of several properties is usually required to determine youth, since many signs may suggest, however not establish by themselves, that a star is young. For M dwarfs, such spectral features can include chromospheric and coronal activity (emission features, in particular strong emission, X-ray emission, flares), signs of accretion discs (e.g. photometric excess, forbidden O I emission lines), Li-absorption in the optical spectrum at 6708Å. Other signs of youth include low surface gravity, low tangential velocity, and kinematic properties consistent with known Young Moving Groups (YMGs) or associations.

Low surface gravity can be measured in medium resolution spectra such as ours for spectral types M5 or later using gravity sensitive alkali lines in the near-infrared (see e.g. Gorlova et al., 2003; McGovern et al., 2004; Kirkpatrick et al., 2006), or by using spectral indices (e.g. Lucas et al., 2001; Kirkpatrick et al., 2006; Allers et al., 2007). We measured the equivalent widths (EW) of the gravity sensitive Na I doublet at 1.138m and the K I doublets at m and m with associated errors as described in Bonnefoy et al. (2014), with the psuedo-continuum wavelength regions reported therein. For a given spectral subtype, low surface gravity, hence youth, can be seen in the reduced strength of the alkali lines compared to main sequence stars. Table LABEL:EW lists the measured EWs for all stars in our sample, with the exception of J040805 and J024902 for which the quality of the spectra was not sufficient for precise measurements. These are also plotted in Fig. 5, together with EWs for field dwarfs from the IRTF SpeX library and 10 Myr old stars from Manara et al. (2013) for comparison. We measured the EWs for all stars in our sample for consistency, even though the only stars in our target sample that are classified as or later are the stars in the GJ 852 BC system and J061610 B. For the latter, the measured Na I at 1.138m is slightly weaker than for the field main sequence template, and the K I at 1.169 and 1.253m overlap with the young template measurement, suggesting intermediate surface gravity. We see no indication of particularly weak alkali lines in the -band spectra for the other targets, and hence no signs of low surface gravity and youth.

No emission lines indicating youth, such as Br or Pa, can be confidently detected in our near-infrared spectra. Weak ‘bumps’ can be seen in the -band spectra of J061345 and J061610 at roughly the position of Pa, however these features likely arise from incomplete H-absorption line subtraction in the telluric spectra during data reduction. Similar ‘bumps’ are seen around the Br absorption feature in -band for GJ 852 BC.

ID NaI (1.138m) KI (1.169m) KI (1.177m) KI (1.243m) KI (1.253m)
(Å) (Å) (Å) (Å) (Å)
J021330 (A)
J021330 (B)
J053018 (A)
J053018 (B)
J061345 (A)
J061345 (B)
J061610 (A)
J061610 (B)
GJ 852 (B)
GJ 852 (C)
Table 4: Equivalent widths of gravity sensitive features.
Figure 5: EWs of surface gravity sensitive features. The SINFONI EWs are shown as yellow diamonds, and compared to EWs measured for IRTF field star templates (dark blue dots) and young stars from the Manara et al. (2013) sample of 10 Myr old stars (light blue triangles).

4 Discussion

4.1 Additional youth indicators

Candidate members of YMGs

Based on the selection of targets from their strong coronal emission and low tangential velocity, Riaz, Gizis & Harvin (2006) estimated that their catalog, from which the AstraLux target sample was obtained, consisted of mainly stars younger than 600 Myr, and using the age-velocity relation of Holmberg, Nordström & Andersen (2009) we derived an upper age for our AstraLux sample of 1 Gyr in Bergfors et al. (2010). Since then, the kinematics of several of our original large survey targets have been investigated for kinematic membership in YMGs and some are candidate members of e.g. the AB Dor Moving Group (MG), the Pic MG, and the Argus and Columba associations (Malo et al., 2013, 2014a; Rodriguez et al., 2013, Schlieder et al., in preparation), including five of our SINFONI targets:

J021330: A convergent point analysis by Rodriguez et al. (2013) yielded a high probability (87%) of Pic MG membership, however, their analysis using the BANYAN statistical software (Malo et al., 2013) placed this target as a field system. The updated BANYAN II web tool (Malo et al., 2013; Gagné et al., 2014), which assumes a refined prior based on the expected populations, places this system as part of the field population. FEROS spectra obtained from the ESO archive show Balmer line and Ca II H & K emission, but no Li-absorption.

J024902: See Sect. 4.1.2.

J053018: This triple system is flagged by Malo et al. (2014a) as a candidate member of the AB Dor MG, with a probability of 97.7% when including radial velocity measurements in the analysis. Using the BANYAN II tool, we find a 73.9% probability of kinematic membership using the refined prior. Additional integrated FEROS spectra show that the system is chromospherically active with strong Balmer line and Ca II H & K emission, however no visible Li-absorption (Bergfors et al., in preparation).

J061345: The binary has 99.99% probability of belonging to the Argus association when radial velocity is included (Malo et al., 2014a), decreasing to 76.1% with the BANYAN II tool. No Li-absorption is visible in integrated FEROS spectra (Bergfors et al., in preparation).

J061610: Using the BANYAN II tool with non-uniform priors, we find a 4% probability that the system belongs to the Pic MG (see also Janson et al., 2014b), while if using uniform prior the probability increases to 99.6%. No radial velocity measurements were included in either analysis. The convergent point analysis tool of Rodriguez et al. (2013) finds a probability of 84% of Pic MG membership.

Our BANYAN II analysis of the GJ 852 and J040805 systems places them as field objects.

FEROS observations of the J024902 system

The CASTOFFS survey to identify young, low-mass stars near the Sun included 2MASS J02490228-1029220 ABC as a candidate of the Pic MG (Schlieder et al., 2012, Schlieder et al. in preparation). The star was selected as a candidate on the basis of consistent position and proper motion, and strong X-ray and UV emission.

Radial and Rotational Velocity: To measure the radial velocity (RV) and rotational velocity of J024902 ABC, we used IDL software to perform a cross-correlation (CC) analysis (Mazeh et al., 2002; Bender & Simon, 2008) with a suite of RV templates taken from Prato et al. (2002). These template stars were observed during FEROS runs in 2011 December and 2012 October and were reduced following the same methods as the science target. We measured the RV of J024902 ABC across portions of four echelle orders chosen to be free of strong telluric absorption. The average RV across the four orders was , where the dominant source of error is a systematic introduced by the use of empirical RV templates. The CC function in each case was strong and single peaked, showing no indication of a tight, spectroscopic binary. The strongest peak was found when using the M2.5 star GJ 752 A as a template. We also measured a projected rotational velocity of v sin i = by cross-correlating our spectrum with rotationally broadened templates.

Spectral type: Our RV analysis indicated that J024902 ABC had a spectral type of from the best match RV template. As a further check, we smoothed our spectrum to and performed a visual comparison to the SDSS M dwarf spectral type templates from The Hammer IDL spectral typing suite (Covey et al., 2007). Although our spectrum is not flux calibrated, our visual comparison of the strength of atomic and molecular absorption features between 5500 and 7000Å yields a spectral type of . We presume this to be the spectral type of the primary, J024902 A, which contributes more flux than the B and C components.

Age indicators and kinematics: The FEROS spectrum of J024902 ABC is rich with emission from the Hydrogen Balmer series () and other signatures of strong magnetic activity. Additionally, the spectrum exhibits strong Li absorption at with  mÅ(see Fig. 6). Taking into account the relative fluxes of an M2 and two M4 components at , the Li strength as a function of temperature, and the Li depletion rate for M2 and M4 dwarfs at ages  Myr (da Silva et al., 2009), we conclude that the only possible contribution to the Li absorption feature must come from the M2 component. In addition, the Li depletion boundary is in between spectral types M4 and M5 in the Pic MG (Binks & Jeffries, 2014; Malo et al., 2014b), and contribution from the lower mass companions is therefore not possible at Pic or older ages. A comparison of our measurement and Li absorption strengths for M1M2 type stars of different ages is shown is Figure 7. The EW of Li in J024902 A is weaker than in M1M2 type members of the  Myr TW Hydrae association, but stronger than members of the Myr old Tucana-Horologium association (Kraus et al., 2014). The Li strength is consistent with that of early-M stars in the Pic MG, suggesting a similar age of  Myr (Mentuch et al., 2008; Mamajek & Bell, 2014).

The position and proper motion of the star combined with our RV measurement reveals that the UVW Galactic velocities of the system are consistent with the Pic group distribution for distances between  pc. However, at these distances J024902 ABC is discrepant with the Pic group XYZ Galactic position distribution by  pc in both X and Z. This is likely why the Bayesian probability estimator BANYAN II provides negligible probability of membership in Pic or any other MG using the available kinematics. Although the combination of consistent partial kinematics and strong evidence for youth make a compelling case for J024902 ABC to be a member of the Pic MG, final group membership assignment will require a parallax measurement and a better understanding of the full XYZ distribution of the Pic group. Nevertheless, the unambiguous detection of Li in the optical spectrum of the system indicates an age  Myr and the system warrants further study.

Figure 6: Li-absorption in FEROS spectrum of J024902 ABC.
Figure 7: Li EW for M1M2 members of the TW Hydrae association (TWA), Pic MG (BP), and Tucana-Horologium association (TUC), from da Silva et al. (2009); Kraus et al. (2014). Individual measurements are plotted as gray open symbols while the means and standard deviations are plotted as larger symbols with error bars. The Li EW and error for the J024902 system, in which the primary contributes all observed Li, is shown as the magenta square. The measured EW is only consistent with similar spectral type members of the Pic MG.

4.2 Hertzsprung-Russell diagram

Comparison with evolutionary models can provide additional constraints on the system ages and mass estimates to be compared to dynamical masses in the future. We compared the positions of the two systems containing components of spectral type M5 or later, J061610 and GJ 852 BC, in a vs. diagram to the Baraffe et al. (2015), hereafter BHAC15, isochrones.

The GJ 852 BC system consists of an M4.5 and an M7.5 star and has a trigonometric parallax of  mas (Harrington & Dahn, 1980). This system is of particular interest for orbital monitoring and age determination, since both young and late-type M dwarf binaries with dynamical masses and well characterised spectra are rare. We measured the -band flux ratio between the BC components and converted to individual apparent magnitudes using integrated 2MASS photometry (Cutri et al., 2003). The individual component absolute -band magnitudes and derived effective temperatures are plotted together with BHAC15 isochrones and iso-mass contours in Fig. 8. Assuming co-evality, the system is likely older than 250 Myr, consistent with the findings from the analysis of gravity sensitive features in the previous section which showed no sign of low surface gravity. For an age  Myr, GJ 852 C has a model mass below the hydrogen burning limit ().

Because of its intermediate surface gravity results in the EW analysis and its debated Pic MG membership (Malo et al., 2013; Janson et al., 2014b), we also put the J061610 system on an H-R diagram, despite its lack of a trigonometric parallax measurement. We assumed the spectroscopic (statistical) distance of  pc derived by Malo et al. (2013) and plot the derived vs. and BHAC15 isochrones in Figure 9. Assuming co-evality and considering the more stringent constraints set by the primary star parameters, we find a system age of  Myr. At this age, both components in the system have masses above the hydrogen burning limit. Various age estimates for the Pic MG in the literature based on different methods such as the lithium depletion boundary, kinematics and ischronal fitting constrains the age to the range  Myr (see e.g. Mamajek & Bell, 2014, for a summary). A system age in this interval can not be rejected from this analysis. We note that for young ages our observed spectral types correspond to higher than we assumed using the Kraus & Hillenbrand (2007) empirical models for Praesepe ( Myr), shifting the stars to the left in the figure and implying a higher age.

Figure 8: Comparison of observed properties of the GJ 852 BC system to the BHAC15 evolutionary models. Isochrones for ages 0.05, 0.10, 0.20, 0.30, 0.50 and 1.0 Gyr are shown as dotted lines; evolutionary sequences for constant mass are shown as solid lines.
Figure 9: Similar to Fig. 8 but for J061610. Isochrones are shown for ages 0.02, 0.03, 0.05, 0.10, 0.20, 0.30, 0.50 and 1.0 Gyr.

5 Summary and conclusions

Our near-infrared spectral analysis of seven close binaries from the AstraLux M dwarf survey provides spectral types for all stars and constraints on surface gravity and age for two systems: GJ 852 BC and J061610. The spectral types derived from visual comparison of spectral energy distribution and absorption features and measuring the Rojas-Ayala et al. (2012) index were found consistent with the estimates determined from colours in the AstraLux M dwarf survey, thereby validating the photometric method. Additional optical spectra of J024902 provides radial and rotational velocity and primary star spectral type as well as age constraints.

The ages of these systems are of particular value for future dynamical mass studies. Upper limits of  Gyr were derived in Bergfors et al. (2010), and lower limits were here explored for the two systems containing components with spectral type M5 or later from EW measurements of gravity sensitive alkali lines and comparison of observed parameters with theoretical isochrones.

From comparison with the BHAC15 evolutionary models we found a lower age limit of  Myr for GJ 852. This intermediate age lower limit is consistent with the analysis of gravity sensitive -band alkali lines and the shape of the spectra, neither of which showed any sign of low gravity and hence ongoing contraction. For an age  Myr we find that the model predicted mass of the C component is below the hydrogen burning limit.

The J061610 system lacks a trigonometric parallax measurement, however, assuming the spectroscopic distance derived by Malo et al. (2013), we found a system age of  Myr. An age consistent with the  Pic MG, in which the system is a kinematic member candidate, can not be ruled out from this analysis. The EW analysis suggests intermediate surface gravity. Future measurements (e.g. the Li EW, radial velocity and trigonometric parallax) would provide firmer constraints on age and model predicted masses.

An analysis of optical spectra and kinematics of the J024902 system suggests an age of  Myr, based on the strong Li absorption. Further data such as parallax is needed to establish membership in the Pic MG.

The ultimate goal of this binary study is to better constrain evolutionary models, which have been shown to systematically under predict masses for objects (Hillenbrand & White, 2004). The AstraLux Large M Dwarf Survey, from which these binaries were selected for spectroscopic characterisation, discovered nearby, low-mass binary systems, many of which belong to YMGs. Ongoing orbital monitoring together with precise parallactic distances obtained with Gaia (Perryman et al., 2001) will within a few years provide dynamical masses for a large number of binaries, providing stringent constraints on evolutionary models for young, low-mass stars.

Acknowledgments

We thank the staff at the Paranal and La Silla observatories for their support, and Jay Farihi and the anonymous referee for useful comments and suggestions.

Footnotes

  1. thanks: Based on observations made with ESO telescopes at the Paranal Observatory under programme IDs 086.A-9014, 086.C-0869, 088.A-9032, 088.C-0753, 089.A-9013 and 091.C-0216.
  2. pagerange: Characterisation of close visual binaries from the AstraLux Large M Dwarf Surveythanks: Based on observations made with ESO telescopes at the Paranal Observatory under programme IDs 086.A-9014, 086.C-0869, 088.A-9032, 088.C-0753, 089.A-9013 and 091.C-0216. References
  3. thanks: Based on observations made with ESO telescopes at the Paranal Observatory under programme IDs 086.A-9014, 086.C-0869, 088.A-9032, 088.C-0753, 089.A-9013 and 091.C-0216.
  4. pubyear: 2015
  5. footnotemark:
  6. footnotemark:
  7. footnotetext: 1
  8. http://www.eso.org/observing/dfo/quality/SINFONI/qc/dark_QC1.html
  9. http://www.eso.org/observing/dfo/quality/SINFONI/qc/qc1.html
  10. The refraction can be corrected by the data reduction pipeline. However, we still noticed some residual drift after this correction had been applied.

References

  1. Abuter, R., Schreiber, J., Eisenhauer, F., Ott, T., Horrobin, M., Gillesen, S., 2006, New Astronomy Reviews, 50, 398
  2. Allers, K. N. et al., 2007, ApJ, 657, 511
  3. Alonso-Floriano, F. J. et al., 2015, A&A, 577, 128
  4. Baraffe, I., Homeier, D., Allard, F., Chabrier, G.,2015, A&A, 577, 42
  5. Bender, C. F., Simon, M., 2008, ApJ, 689, 416
  6. Bergfors, C. et al., 2010, A&A, 520, A54
  7. Binks, A. S., Jeffries, R. D., 2014, MNRAS, 438, L11
  8. Bochanski, J. J., West, A. A., Hawley, S. L., Covey, K. R., 2007, AJ, 133, 531
  9. Bonnefoy, M. et al., 2009, A&A, 506, 799
  10. Bonnefoy, M., Chauvin, G., Lagrange, A.-M., Rojo, P., Allard, F., Pinte, C., Dumas, C., Homeier, D., 2014, A&A, 562, 127
  11. Bonnet, H. et al., 2003, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 4839, 329
  12. Bonnet, H. et al., 2004, The Messenger, 117, 17
  13. Bouy, H. et al., 2008, A&A, 481, 757
  14. Bowler, B. P., Liu, M. C., Shkolnik, E. L., Tamura, M., 2015, ApJS, 216, 7
  15. Burgasser, A. J., Reid, I. N., Siegler, N., Close, L., Allen, P., Lowrance, P., Gizis, J., 2007, in Reipurth, B., Jewitt, D., Keil, K., eds, Protostars and Planets V, Not Alone: Tracing the Origins of Very-Low-Mass Stars and Brown Dwarfs Through Multiplicity Studies. pp 427–441
  16. Close, L. M. et al., 2005, Nature, 433, 286
  17. Covey, K. R. et al., 2007, AJ, 134, 2398
  18. Covey, K. R., Lada, C. J., Román-Zúñiga, C., Muench, A. A., Forbrich, J., Ascenso, J., 2010, ApJ, 722, 971
  19. Cushing, M. C., Rayner, J. T., Vacca, W. D., 2005, ApJ, 623, 1115
  20. Cutri, R. M. et al.. 2003, VizieR Online Data Catalog II/246
  21. Daemgen, S., Hormuth, F., Brandner, W., Bergfors, C., Janson, M., Hippler, S., Henning, T., 2009, A&A, 498, 567
  22. da Silva, L., Torres, C. A. O., de La Reza, R., Quast, G. R., Melo, C. H. F., Sterzik, M. F., 2009, A&A, 508, 833
  23. Dressing, C. D., Charbonneau, D., 2013, ApJ, 767, 95
  24. Duchêne, G., Kraus, A., 2013, ARA&A, 51, 269
  25. Dumas, C., Terrile, R. J., Brown, R. H., Schneider, G., Smith, B. A., 2001, AJ, 121, 1163
  26. Dupuy, T. J., Liu, M. C., Bowler, B. P., Cushing, M. C., Helling, C., Witte, S., Hauschildt, P., 2010, ApJ, 721, 1725
  27. Eisenhauer, F. et al., 2003, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, 4841, 1548
  28. Gagné, J., Lafrenière, D., Doyon, R., Malo, L., Artigau, É., 2014, ApJ, 783, 121
  29. Gaidos, E. et al., 2014, MNRAS, 443, 2561
  30. Goodwin, S. P., Kroupa, P., Goodman, A., Burkert, A., 2007, in Reipurth, B., Jewitt, D., Keil, K., eds, Protostars and Planets V, Not Alone: Tracing the Origins of Very-Low-Mass Stars and Brown Dwarfs Through Multiplicity Studies. pp 133-147
  31. Gorlova, N. I., Meyer, M. R., Rieke, G. H., Liebert, J.,2003, ApJ, 593, 1074
  32. Harrington, R. S. and Dahn, C. C., 1980, AJ, 85, 454
  33. Hillenbrand, L. A., White, R. J., 2004, ApJ, 604, 741
  34. Holmberg, J., Nordström, B., Andersen, J., 2009, A&A, 501, 941
  35. Janson, M., Brandner, W., Lenzen, R., Close, L., Nielsen, E., Hartung, M., Henning, T., Bouy, H., 2007, A&A, 462, 615
  36. Janson, M. et al., 2012, ApJ, 754, 44
  37. Janson, M. et al., 2014a, ApJ, 789, 102
  38. Janson, M. et al., 2014b, ApJS, 214, 17
  39. Johnson, J. A. et al., 2012, AJ, 143,111
  40. Kaufer, A.,Stahl, O., Tubbesing, S., Nørregaard, P., Avila, G., Francois, P., Pasquini, L., Pizzella, A., 1999, The Messenger, 95, 8
  41. Kirkpatrick, J. D., Barman, T. S., Burgasser, A. J., McGovern, M. R., McLean, I. S., Tinney, C. G., Lowrance, P. J., 2006, ApJ, 639, 1120
  42. Konopacky, Q. M. et al., 2010, ApJ, 711, 1087
  43. Kraus, A. L., Hillenbrand, L. A., 2007, AJ, 134, 2340
  44. Kraus, A. L., Shkolnik, E. L., Allers, K. N., Liu, M. C., 2014, AJ, 147, 146
  45. Lucas, P. W., Roche, P. F., Allard, F., Hauschildt, P. H., 2001, MNRAS, 326, 695
  46. Malo, L. et al., 2013, ApJ, 762, 88
  47. Malo, L., Artigau, É., Doyon, R., Lafrenière, D., Albert, L., Gagné, J., 2014a, ApJ, 788, 81
  48. Malo, L., Doyon, R., Feiden, G. A., Albert, L., Lafrenière, D., Artigau, É., Gagné, J., Riedel, A., 2014b, ApJ, 792, 37
  49. Mamajek, E. E. and Bell, C. P. M., 2014, MNRAS, 445, 2169
  50. Manara, C. F. et al., 2013, A&A, 551, 107
  51. Mann, A. W., Gaidos, E., Lépine, S., Hilton, E. J., 2012, ApJ, 753, 90
  52. Mann, A. W., Gaidos, E., Ansdell, M., 2013, ApJ, 779, 188
  53. Mann, A. W., Gaidos, E., Kraus, A., Hilton, E. J., 2013, ApJ, 770, 43
  54. Mazeh, T., Prato, L., Simon, M., Goldberg, E., Norman, D., Zucker, S., 2002, ApJ, 564, 1007
  55. McGovern, M. R., Kirkpatrick, J. D., McLean, I. S., Burgasser, A. J., Prato, L., Lowrance, P. J., 2004, ApJ, 600, 1020
  56. Mentuch, E., Brandeker, A., van Kerkwijk, M. H., Jayawardhana, R., Hauschildt, P. H., 2008, ApJ, 689, 1127
  57. Muirhead, P. S., Hamren, K., Schlawin, E., Rojas-Ayala, B., Covey, K. R., Lloyd, J. P., 2012, ApJ, 750, 37
  58. Muirhead, P. S. et al., 2014, ApJS, 213, 5
  59. Newton, E. R., Charbonneau, D., Irwin, J., Berta-Thompson, Z. K., Rojas-Ayala, B., Covey, K. and Lloyd, J. P., 2014, AJ, 147, 20
  60. Newton, E. R., Charbonneau, D., Irwin, J., Mann, A. W., 2015, ApJ, 800, 85
  61. Perryman, M. A. C. et al., 2001, A&A, 369, 339
  62. Prato, L., Simon, M., Mazeh, T., McLean, I. S., Norman, D., Zucker, S., 2002, ApJ, 569, 863
  63. Rayner, J. T., Cushing, M. C., Vacca, W. D., 2009, ApJS, 185, 289
  64. Riaz, B., Gizis, J. E., Harvin, J., 2006, AJ, 132, 866
  65. Rodriguez, D. R., Zuckerman, B., Kastner, J. H., Bessell, M. S., Faherty, J. K., Murphy, S. J., 2013, ApJ, 774, 101
  66. Rojas-Ayala, B., Covey, K. R., Muirhead, P. S., Lloyd, J. P., 2012, ApJ, 748, 93
  67. Schlieder, J. E., Lépine, S., Simon, M., 2012, AJ, 143, 80
  68. Schlieder, J. E., 2014, ApJ, 783, 27
  69. Zhou, G. et al., 2014, MNRAS, 437, 2831
248420
This is a comment super asjknd jkasnjk adsnkj
Upvote
Downvote
Edit
-  
Unpublish
""
The feedback must be of minumum 40 characters
The feedback must be of minumum 40 characters
Submit
Cancel
Comments 0
Request comment
""
The feedback must be of minumum 40 characters
Add comment
Cancel
Loading ...

You are asking your first question!
How to quickly get a good answer:
  • Keep your question short and to the point
  • Check for grammar or spelling errors.
  • Phrase it like a question
Test
Test description