arXiv subjects

R. Rebolo

Publications and source records attributed to R. Rebolo.

286 records · Page 16Linked to original sources

arXiv1998

Boron in Very Metal-Poor Stars

We have observed the B I 2497 A line to derive the boron abundances of two very metal-poor stars selected to help in tracing the origin and evolution of this element in the early Galaxy: BD +23 3130 and HD 84937. The observations were conducted using the Goddard High Resolution Spectrograph on board the Hubble Space Telescope. A very detailed abundance analysis via spectral synthesis has been carried out for these two stars, as well as for two other metal-poor objects with published spectra, using both Kurucz and OSMARCS model photospheres, and taking into account consistently the NLTE effects on the line formation. We have also re-assessed all published boron abundances of old disk and halo unevolved stars. Our analysis shows that the combination of high effective temperature (Teff > 6000 K, for which boron is mainly ionized) and low metallicity ([Fe/H]<-1) makes it difficult to obtain accurate estimates of boron abundances from the B I 2497 A line. This is the case of HD 84937 and three other published objects (including two stars with [Fe/H] ~ -3), for which only upper limits can be established. BD +23 3130, with [Fe/H] ~ -2.9 and logN(B)_NLTE=0.05+/-0.30, appears then as the most metal-poor star for which a firm measurement of the boron abundance presently exists. The evolution of the boron abundance with metallicity that emerges from the seven remaining stars with Teff < 6000 K and [Fe/H]<-1, for which beryllium abundances were derived using the same stellar parameters, shows a linear increase with a slope ~ 1. Furthermore, the B/Be ratio found is constant at a value ~ 20 for stars in the range -3<[Fe/H]<-1. These results point to spallation reactions of ambient protons and alpha particles with energetic particles enriched in CNO as the origin of boron and beryllium in halo stars.

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arXiv1997

The IAC-Bartol Cosmic Microwave Background Anisotropy Experiment: Results of the 1994 Campaign

We present the results of a Cosmic Microwave Background (CMB) anisotropy ground-based millimetric experiment sensitive to fluctuations on angular scales of $\sim 2\degg$. Four independent bands centered at 3.3, 2.1, 1.3 and 1.1 mm collected $\sim 550$ hours of observation during the Summer of 1994. The instrument was located on the island of Tenerife at an altitude of 2400 m. The low water-vapor content and the atmospheric stability of the site, combined with new techniques to subtract atmospheric noise, result in the reduction of atmospheric contamination in the lowest frequency channel to a level of $\sim 1.5$~times the instrument noise. Detailed estimations of Galactic foreground contamination show that this contribution is negligible at $|b| \stackrel{>}{_\sim} 12\degg$. Two different multipole bands ($\ell=53^{+22}_{-13}$ and $33^{+24}_{-13}$) are analyzed showing that our technique to subtract the atmospheric contribution is more effective in the multipole band at $\ell=53$. A likelihood analysis of these data reveals the presence of a common signal between the channels at 3.3, 2.1 and 1.3 mm corresponding to a band power estimate of $ \sqrt{\lla (\lla+1) C_{\lla}/(2 π)} = 2.0^{+1.0}_{-0.8} \cdot 10^{-5}$ and $\sqrt{\lla (\lla+1) C_{\lla}/(2 π)} = 4.1^{+2.4}_{-2.2} \cdot 10^{-5}$ for the $\ell =53$ and 33 multipole bands respectively. Calibration uncertainty has been treated as a systematic effect. The level of fluctuations in the $\ell =53$ band is in good agreement with our preliminary analysis presented in Piccirillo \et 1997, with measurements by other experiments working at similar angular scales, and with the predictions of standard Cold Dark Matter (CDM) models.

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arXiv1997

New Brown Dwarfs in the Pleiades Cluster

We present intermediate and low resolution optical spectroscopy (650-915 nm) of seven faint, very red objects (20 > I >= 17.8, I-Z >= 0.5) discovered in a CCD-based IZ survey covering an area of 1 sq. deg in the central region of the Pleiades open cluster. The observed spectra show that these objects are very cool dwarfs, having spectral types in the range M6-M9. Five out of the seven objects can be considered as Pleiades members on the basis of their radial velocities, Halpha emission and other gravity sensitive atomic features like the NaI doublet at 818.3 and 819.5 nm. According to current evolutionary models the masses of these new objects range from roughly 80 MJup for the hottest in the sample down to 45 MJup for Roque 4, the coolest and faintest confirmed member. These observations prove that the cloud fragmentation process extends well into the brown dwarf realm, suggesting a rise in the initial mass function below the substellar limit.

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arXiv1997

Beryllium, Lithium and Oxygen Abundances in F-type Stars

Beryllium and oxygen abundances have been derived in a sample of F-type field stars for which lithium abundances had been measured previously, with the aim of obtaining observational constraints to discriminate between the different mixing mechanisms proposed. Mixing associated with the transport of angular momentum in the stellar interior and internal gravity waves within the framework of rotating evolutionary models, appear to be promising ways to explain the observations.

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arXiv1997

Studies of CMB structure at Dec=40. II: Analysis and cosmological interpretation

We present a detailed analysis of the cosmic microwave background structure in the Tenerife Dec=+40 degrees data. The effect of local atmospheric contributions on the derived fluctuation amplitude is considered, resulting in an improved separation of the intrinsic CMB signal from noise. Our analysis demonstrates the existence of common structure in independent data scans at 15 and 33 GHz. For the case of fluctuations described by a Gaussian auto-correlation function, a likelihood analysis of our combined results at 15 and 33 GHz implies an intrinsic rms fluctuation level of 48^{+21}_{-15} uK on a coherence scale of 4 degrees; the equivalent analysis for a Harrison-Zel'dovitch model gives a power spectrum normalisation of Q_{rms-ps} = 22^{+10}_{-6} uK. The fluctuation amplitude is seen to be consistent at the 68% confidence level with that reported for the COBE two-year data for primordial fluctuations described by a power law model with a spectral index in the range 1.0 \le n \le 1.6. This limit favours the large scale CMB anisotropy being dominated by scalar fluctuations rather than tensor modes from a gravitational wave background. The large scale Tenerife and COBE results are considered in conjunction with observational results from medium scale experiments in order to place improved limits on the fluctuation spectral index; we find n=1.10 +/- 0.10 assuming standard CDM with H_{0}=50 kms^{-1}Mpc^{-1}.

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arXiv1997

New Cosmological Structures on Medium Angular Scales Detected with the Tenerife Experiments

We present observations at 10 and 15 GHz taken with the Tenerife experiments in a band of the sky at Dec.=+35 degrees. These experiments are sensitive to multipoles in the range l=10-30. The sensitivity per beam is 56 and 20 microK for the 10 and the 15 GHz data, respectively. After subtraction of the prediction of known radio-sources, the analysis of the data at 15 GHz at high Galactic latitude shows the presence of a signal with amplitude Delta Trms ~ 32 microK. In the case of a Harrison-Zeldovich spectrum for the primordial fluctuations, a likelihood analysis shows that this signal corresponds to a quadrupole amplitude Q_rms-ps=20.1+7.1-5.4 microK, in agreement with our previous results at Dec.+=40 degrees and with the results of the COBE DMR. There is clear evidence for the presence of individual features in the RA range 190 degrees to 250 degrees with a peak to peak amplitude of ~110 microK. A preliminary comparison between our results and COBE DMR predictions for the Tenerife experiments clearly indicates the presence of individual features common to both. The constancy in amplitude over such a large range in frequency (10-90 GHz) is strongly indicative of an intrinsic cosmological origin for these structures.

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arXiv1997

Brown Dwarfs in the Pleiades Cluster. II. J, H and K photometry

We have obtained near-IR observations of some of the faintest objects so far known towards the Pleiades cluster, with the aim of investigating the sequence that connects cluster very low-mass (VLM) stars with substellar objects. We find that IR data combined with optical magnitudes are a useful tool to discriminate cluster members from foreground/background late-type field stars contaminating optical surveys. The bottom of the Pleiades sequence is clearly defined by the faint HHJ objects as the VLM stars approaching the substellar limit (SL), by the transition object PPl15, which will barely ignite its H content, and by the two brown dwarfs (BDs) Calar3 and Teide1. Binarity amongst cluster members could account for the large dispersion observed in the faint end of the IR colour- magnitude diagrams. Two objects in our sample, namely HHJ6 and PPl15, are overluminous compared to other members, suggesting probable binarity. We have reproduced the photometric measurements of both of them by combining the magnitudes of cluster VLM stars and BDs and using the most recent theoretical evolutionary tracks. The likely masses of the components are slightly above the SL for HHJ6, while they are 0.080 and 0.045+-0.010 Msun for PPl15. These masses are consistent with the constraints imposed by the published Li observations of these Pleiads. We find a single object IR sequence in the Pleiades connecting VLM stars and BDs. We propose that the SL (~0.075 Msun) in the Pleiades (~120 Myr) takes place at absolute magnitudes M(I,J,H,K)=12.4, 10.1, 9.4, 9.0 (~M7). Cluster members fainter by 0.2mag in I and by 0.1mag in K should be proper BDs. The star-BD frontier in the Hyades would be located at M(I,J,H,K)=15.0, 11.6, 10.8, 10.4 (~M9). For ages older than 1000 Myr we estimate that BDs are fainter than M(K)=10.9 (later than M9.5).

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arXiv1996

Millimetric Ground-based Observations of Cosmic Microwave Background Anisotropy

First results of a Cosmic Microwave Background (CMB) anisotropy experiment conducted at the Observatorio del Teide (Tenerife, Spain) are presented. The instrument is a four channel (3.1, 2.1, 1.3 and 1.1 mm) $^3$He bolometer system coupled to a 45 cm diameter telescope. The resultant configuration is sensitive to structures on angular scales ~ 1-2 degrees. We use the channels at the two highest frequencies for monitoring the atmosphere, and apply a simple method to subtract this contribution in channels 1 (3.1 mm) and 2 (2.1 mm). The most intense structure at these two frequencies is the Galactic crossing with peak amplitudes of ~ 350 micro-K. These crossings have been clearly detected with the amplitude and shape predicted. This demonstrates that our multifrequency observations allow an effective assessment and subtraction of the atmospheric contribution. In the section of data at high Galactic latitude we obtain sensitivities ~ 40 micro-K per beam. The statistical analyses show the presence of common signals between channels 1 and 2. Assuming a simple Gaussian auto-correlation model with a scale of coherence $θ_c=1.32$ degrees for the signal, a likelihood analysis of this section of data reveals the presence of fluctuations with intrinsic amplitude $C_{0}^{1/2} = 76^{+43}_{-32}$ micro -K (68 % CL including a ~ 20% calibration uncertainty). Since residual atmospheric noise might still contaminate our results, we also give our result as an upper limit of 118 micro-K at 95% c.l.

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arXiv1996

Brown Dwarfs in the Pleiades Cluster Confirmed by the Lithium Test

We present 10 m Keck spectra of the two Pleiades brown dwarfs Teide 1 and Calar 3 showing a clear detection of the 670.8 nm Li resonance line. In Teide 1, we have also obtained evidence for the presence of the subordinate line at 812.6 nm. A high Li abundance (log N(Li) >= 2.5), consistent with little if any depletion, is inferred from the observed lines. Since Pleiades brown dwarfs are unable to burn Li the significant preservation of this fragile element confirms the substellar nature of our two objects. Regardless of their age, their low luminosities and Li content place Teide 1 and Calar 3 comfortably in the genuine brown dwarf realm. Given the probable age of the Pleiades cluster, their masses are estimated at 55 +- 15 Jupiter masses.

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arXiv1996

Brown Dwarfs in the Pleiades Cluster: a CCD-based R,I survey

We have obtained deep CCD R and I mosaic imaging of 578 arcmin$^{2}$ within 1$^{\circ}$.5 of the Pleiades' center -- reaching a completeness magnitude I=19.5 -- with the aim of finding free-floating brown dwarfs. Teide~1, the best $bona$ $fide$ brown dwarf discovered so far in the cluster (Rebolo, Zapatero Osorio \& Mart\'ın 1995), arose as a result of a combined photometric and astrometric study of $\sim$1/4 of our covered area. The extension of our two-colour survey provides eight new additional brown dwarf candidates whose photometry is rather similar to that of Teide~1. Several of them are even fainter. Follow up low-resolution spectroscopy (Mart\'ın, Rebolo \& Zapatero Osorio 1996) shows that one of them is indeed a Pleiades brown dwarf. Most of the remaining candidates are background late-M dwarfs which are contaminating our survey, possibly due to a small (previously unknown) cloud towards the cluster which affects some of our CCD fields. We did not expect any foreground M8--M9 field dwarf in our surveyed volume and surprisingly we have found one, suggesting that its number could be larger than inferred from recent luminosity function studies in the solar neighbourhood.

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arXiv1996

Spectroscopy of New Substellar Candidates in the Pleiades: Towards a Spectral Sequence for Young Brown Dwarfs

We present optical and near-IR spectroscopy (600--1000 nm) of 8 faint (I$>$18) very red (R--I$>$2.2) objects discovered in a deep CCD survey of the Pleiades (Zapatero-Osorio et al. 1996). We compare them with reliable cluster members like PPl 15 and Teide 1, and with several field very late-type dwarfs (M4--M9.5), which were observed with similar instrumental configurations. Using pseudocontinuum ratios we classify the new substellar candidates in a spectal sequence defined with reference to field stars of known spectral types. We also reclassify PPl 15 and Teide 1 in a self-consistent way. The likelihood of membership for the new candidates is assesed via the study of their photospheric features, Ha emission, radial velocity, and consistency of their spectral types and I magnitudes with known cluster members. Four of the new substellar candidates are as late or later than PPl~15 (M6.5), but only one, Calar 3 (M8), clearly meets all our membership criteria. It is indeed an object very similar to the brown dwarf Teide 1. Calar 3, together with Teide 1, allows one to compare the spectroscopic characteristics of Pleiades brown dwarfs with those of old very cool dwarfs. The overall spectral properties are similar, but there are slight differences in the NaI doublet (818.3 nm, 819.5 nm), VO molecular band (740 nm), and some spectral ratios, which are probably related to lower surface gravity in the young Pleiades brown dwarfs than in field stars. Finally, we propose a way of improving future CCD-based brown dwarf surveys by using narrow-band near-IR pseudocontinuum filters.

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arXiv1995

Stars Approaching the Substellar Limit in the alpha Persei Open Cluster

We present intermediate dispersion optical spectroscopy for seven very low-mass stars in the alpha Per open cluster with spectral types between M3 and M6, including the brown dwarf candidate of Rebolo et al. (1992). Our radial velocity measurements are found to be generally consistent with the mean cluster velocity to within the measurement errors. Halpha equivalent widths have been measured and compared to previous published data for other known members of the cluster. A turnover in chromospheric activity around spectral type M3-M4 is observed. The brown dwarf candidate, located in the cool side of the turnover, is confirmed to exhibit a strong Halpha variability. It is the coolest alpha Per candidate member for which spectra are available and for which chromospheric activity has been measured. Using the LiI doublet at lambda 6707.8 angstroms, we derive upper limits to the atmospheric Li abundance in the sample and discuss them in the context of the most recent stellar evolutionary tracks. The non-detection of the LiI line in the spectrum of the brown dwarf candidate implies a mass greater than 0.08 solar masses, and therefore it is not a substellar object. However, its position in the HR diagram implies that this star is indeed very close to the substellar limit.

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arXiv1994

Comparison of the COBE DMR and Tenerife Data

We have compared the Tenerife data with the {\it COBE} DMR two-year data in the declination +40°region of the sky observed by the Tenerife experiment. Using the Galactic plane signal at $\sim 30$ GHz, we show that the two data sets are cross-calibrated to within 5%. The high Galactic latitude data were investigated for the presence of common structures with the properties of cosmic microwave background (CMB) fluctuations. The most prominent feature in the Tenerife data ($ΔT \sim 80μ$K) is evident in both the 53 and 90 GHz DMR maps and has the Planckian spectrum expected for CMB anisotropy. The cross-correlation function of the Tenerife and DMR scans is indicative of common structure and at zero lag has the value $C(0)^{1/2}=34^{+13}_{-15}\: μ$K. The combination of the spatial and spectral information from the two data sets is consistent with the presence of cosmic microwave background anisotropies common to both. The probability that noise could produce the observed agreement is less than 5%.

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arXiv1994

Lithium and the Nature of Brown Dwarf Candidates

This paper discusses the ability of Li to confirm the substellar nature of a brown dwarf candidate. Theoretical computations using different interior models agree that brown dwarfs with masses below $\sim$ 0.065 M$_{\odot}$ preserve a significant fraction of their initial Li content while for higher masses total Li depletion occurs in very short timescales. Refined spectral synthesis using brown dwarf model atmospheres shows that the Li I resonance line at 670.8 nm should produce a conspicuous feature at effective temperatures higher than 2000 K, suitable for spectroscopic detection in present brown dwarf candidates. We summarize the results of our search for Li in many of the best candidates known so far.

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arXiv1994

Constraints to the Masses of Brown Dwarf Candidates from the Lithium Test

We present intermediate dispersion (0.7-2.2 Å~pix$^{-1}$) optical spectroscopic observations aimed at applying the ``Lithium Test'' to a sample of ten brown dwarf candidates located in the general field, two in young open clusters, and two in close binaries. We find evidence for strong Li depletion in all of them, and thus infer lower mass limits of 0.065~M$_\odot$, depending only slightly ($\pm$0.005~M$_\odot$) on the interior models. None of the field brown dwarf candidates in our sample appears to be a very young (age $<$~10$^8$~yr) substellar object. For one of the faintest proper motion Pleiades members known (V=20.7) the Li test implies a mass greater than $\sim$0.08~M$_\odot$, and therefore it is not a brown dwarf. From our spectra we estimate spectral types for some objects and present measurements of Halpha emission strengths and radial velocities. Finally, we compare the positions in the H-R diagram of our sample of brown dwarf candidates with the theoretical region where Li is expected to be preserved (Substellar Lithium Region). We find that certain combinations of temperature calibrations and evolutionary tracks are consistent with the constraints imposed by the observed Li depletion in brown dwarf candidates, while others are not.

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arXiv1993

Pre-main sequence lithium burning. I. Weak T Tauri stars

We derive lithium abundances in 53 T Tauri stars (TTS), concentrating on weak-line TTS. Our study gives the following results: 1)At luminosities $\ge 0.9 L\sun$ the Li abundances are remarkably uniform, with a mean value, log~N(Li)=3.1, equal to the "cosmic" lithium abundance. 2)Significant Li depletion appears below 0.5~L$\sun$ in the mass range 0.9-0.2 M$\sun$ and increases towards lower luminosities. At the lower mass end (0.4-0.2 M$\sun$), the observed luminosity of the Li burning turning point is about a factor 4 higher than predicted by the models. At masses 1.2-1.0 M$\sun$ the observations imply less PMS Li burning than theoretically expected. Moreover we show that: 1)Low Li abundances appear only among stars with low $v\sin{i}$. Fast rotators with masses around 0.8~M$\sun$ do not show evidence for strong Li depletion towards lower luminosities as slow rotators do. 2)In a sample restricted to only K5-K7 stars we find that the angular momentum spread before Li burning begins is larger than a factor 10. Lithium depletion associated to angular momentum loss during PMS evolution is not required to explain the observed abundances. The efficiency of PMS Li burning in the mass range 0.9-0.7~M$\sun$ is reduced in the presence of rapid rotation.

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