J. Neill, M. Sullivan, M. D. W. U. O. Technology, U. Oxford, C. Observatories
We exploit the accumulating, high‐quality, multi‐wavelength imaging data of nearby supernova (SN) hosts to explore the relationship between SN production and host galaxy evolution. The Galaxy Evolution Explorer (GALEX, [1]) provides ultraviolet (UV) imaging in two bands, complementing data in the optical and infra‐red (IR). We compare host properties, derived from spectral energy distribution (SED) fitting, with nearby, well‐observed SN Ia light curve properties. We also explore where the hosts of different types of SNe fall relative to the red and blue sequences on the galaxy UV‐optical color‐magnitude diagram (CMD, [2]). We conclude that further exploration and larger samples will provide useful results for constraining the progenitors of SNe.
{"title":"The GALEX View of Supernova Hosts","authors":"J. Neill, M. Sullivan, M. D. W. U. O. Technology, U. Oxford, C. Observatories","doi":"10.1063/1.3141604","DOIUrl":"https://doi.org/10.1063/1.3141604","url":null,"abstract":"We exploit the accumulating, high‐quality, multi‐wavelength imaging data of nearby supernova (SN) hosts to explore the relationship between SN production and host galaxy evolution. The Galaxy Evolution Explorer (GALEX, [1]) provides ultraviolet (UV) imaging in two bands, complementing data in the optical and infra‐red (IR). We compare host properties, derived from spectral energy distribution (SED) fitting, with nearby, well‐observed SN Ia light curve properties. We also explore where the hosts of different types of SNe fall relative to the red and blue sequences on the galaxy UV‐optical color‐magnitude diagram (CMD, [2]). We conclude that further exploration and larger samples will provide useful results for constraining the progenitors of SNe.","PeriodicalId":8453,"journal":{"name":"arXiv: Astrophysics","volume":"1 1","pages":"528-531"},"PeriodicalIF":0.0,"publicationDate":"2008-12-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"85798475","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
A fraction of neutrino emission from GRB accretion disks annihilates above the disk, creating e± plasma that can drive GRB explosions. We calculate the efficiency of this annihilation using the recent detailed model of hyper‐accretion disks around Kerr black holes. Our calculation is fully relativistic and based on a geodesic‐tracing method. We find that the efficiency is a well‐defined function of (1) accretion rate and (2) spin of the black hole. It is practically independent of the details of neutrino transport in the opaque zone of the disk. The results help identify the accretion disks whose neutrino emission can power GRBs.
{"title":"Efficiency of Neutrino Annihilation around Spinning Black Holes","authors":"I. Zalamea, A. Beloborodov","doi":"10.1063/1.3155863","DOIUrl":"https://doi.org/10.1063/1.3155863","url":null,"abstract":"A fraction of neutrino emission from GRB accretion disks annihilates above the disk, creating e± plasma that can drive GRB explosions. We calculate the efficiency of this annihilation using the recent detailed model of hyper‐accretion disks around Kerr black holes. Our calculation is fully relativistic and based on a geodesic‐tracing method. We find that the efficiency is a well‐defined function of (1) accretion rate and (2) spin of the black hole. It is practically independent of the details of neutrino transport in the opaque zone of the disk. The results help identify the accretion disks whose neutrino emission can power GRBs.","PeriodicalId":8453,"journal":{"name":"arXiv: Astrophysics","volume":"11 1","pages":"121-123"},"PeriodicalIF":0.0,"publicationDate":"2008-12-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"85866070","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2008-12-21DOI: 10.1051/0004-6361/200811256
A. Rutkowski, A. Olech, M. Wi'sniewski, P. Pietrukowicz, J. Pala, Radosław Poleski
We report an analysis of photometric behaviour of DI UMa, an extremely active dwarf nova. The observational campaign (completed in 2007) covers five superoutbursts and four normal outbursts. We examined principal parameters of the system to understand peculiarities of DI UMa, and other active cataclysmic variables. Based on precise photometric measurements, temporal light curve behaviour, O-C analysis, and power spectrum analysis, we investigated physical parameters of the system. We found that the period of the supercycle now equals 31.45 +/-0.3 days. Observations during superoutbursts infer that the period of superhumps equals P_sh = 0.055318(11) days (79.66 +/- 0.02 min). During quiescence, the light curve reveals a modulation of period P_orb = 0.054579(6) days (78.59 +/- 0.01 min), which we interpret as the orbital period of the binary system. The values obtained allowed us to determine a fractional period excess of 1.35% +/- 0.02%, which is surprisingly small compared to the usual value for dwarf novae (2%-5%). A detailed O-C analysis was performed for two superoutbursts with the most comprehensive coverage. In both cases, we detected an increase in the superhump period with a mean rate of dot_P/P_sh = 4.4(1.0)*10^{-5}. Based on these measurements, we confirm that DI UMa is probably a period bouncer, an old system that reached its period minimum a long time ago, has a secondary that became a degenerate brown dwarf, the entire system evolving now toward longer periods. DI UMa is an extremely interesting object because we know only one more active ER UMa star with similar characteristics (IX Dra).
{"title":"Curious Variables Experiment (CURVE). CCD photometry of active dwarf nova DI UMa","authors":"A. Rutkowski, A. Olech, M. Wi'sniewski, P. Pietrukowicz, J. Pala, Radosław Poleski","doi":"10.1051/0004-6361/200811256","DOIUrl":"https://doi.org/10.1051/0004-6361/200811256","url":null,"abstract":"We report an analysis of photometric behaviour of DI UMa, an extremely active dwarf nova. The observational campaign (completed in 2007) covers five superoutbursts and four normal outbursts. We examined principal parameters of the system to understand peculiarities of DI UMa, and other active cataclysmic variables. Based on precise photometric measurements, temporal light curve behaviour, O-C analysis, and power spectrum analysis, we investigated physical parameters of the system. We found that the period of the supercycle now equals 31.45 +/-0.3 days. Observations during superoutbursts infer that the period of superhumps equals P_sh = 0.055318(11) days (79.66 +/- 0.02 min). During quiescence, the light curve reveals a modulation of period P_orb = 0.054579(6) days (78.59 +/- 0.01 min), which we interpret as the orbital period of the binary system. The values obtained allowed us to determine a fractional period excess of 1.35% +/- 0.02%, which is surprisingly small compared to the usual value for dwarf novae (2%-5%). A detailed O-C analysis was performed for two superoutbursts with the most comprehensive coverage. In both cases, we detected an increase in the superhump period with a mean rate of dot_P/P_sh = 4.4(1.0)*10^{-5}. Based on these measurements, we confirm that DI UMa is probably a period bouncer, an old system that reached its period minimum a long time ago, has a secondary that became a degenerate brown dwarf, the entire system evolving now toward longer periods. DI UMa is an extremely interesting object because we know only one more active ER UMa star with similar characteristics (IX Dra).","PeriodicalId":8453,"journal":{"name":"arXiv: Astrophysics","volume":"152 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2008-12-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"86222816","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
I review some of the findings on the Magellanic System produced by the Far Ultraviolet Spectroscopic Explorer (FUSE) during and after its eight years of service. The Magellanic System with its high‐velocity complexes provides a nearby laboratory that can be used to characterize phenomena that involve interaction between galaxies, infall and outflow of gas and metals in galaxies. These processes are crucial for understanding the evolution of galaxies and the intergalactic medium. Among the FUSE successes I highlight are the coronal gas about the LMC and SMC, and beyond in the Stream, the outflows from these galaxies, the discovery of molecules in the diffuse gas of the Stream and the Bridge, an extremely sub‐solar and sub‐SMC metallicity of the Bridge, and a high‐velocity complex between the Milky Way and the Clouds.
{"title":"The Magellanic System: What have we learnt from FUSE?","authors":"N. Lehner","doi":"10.1063/1.3154068","DOIUrl":"https://doi.org/10.1063/1.3154068","url":null,"abstract":"I review some of the findings on the Magellanic System produced by the Far Ultraviolet Spectroscopic Explorer (FUSE) during and after its eight years of service. The Magellanic System with its high‐velocity complexes provides a nearby laboratory that can be used to characterize phenomena that involve interaction between galaxies, infall and outflow of gas and metals in galaxies. These processes are crucial for understanding the evolution of galaxies and the intergalactic medium. Among the FUSE successes I highlight are the coronal gas about the LMC and SMC, and beyond in the Stream, the outflows from these galaxies, the discovery of molecules in the diffuse gas of the Stream and the Bridge, an extremely sub‐solar and sub‐SMC metallicity of the Bridge, and a high‐velocity complex between the Milky Way and the Clouds.","PeriodicalId":8453,"journal":{"name":"arXiv: Astrophysics","volume":"196 1","pages":"29-33"},"PeriodicalIF":0.0,"publicationDate":"2008-12-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"76967396","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2008-12-20DOI: 10.1088/0004-6256/137/3/3718
M. Lister, H. Aller, M. Aller, M. Cohen, D. Homan, M. Kadler, K. Kellermann, Y. Y. Kovalev, E. Ros, T. Savolainen, J. Zensus, R. Vermeulen
We present images from a long term program (MOJAVE: Monitoring of Jets in AGN with VLBA Experiments) to survey the structure and evolution of parsec-scale jet phenomena associated with bright radio-loud active galaxies in the northern sky. The observations consist of 2424 15 GHz VLBA images of a complete flux-density limited sample of 135 AGN above declination -20 degrees, spanning the period 1994 August to 2007 September. These data were acquired as part of the MOJAVE and 2 cm Survey programs, and from the VLBA archive. The sample selection criteria are based on multi-epoch parsec-scale (VLBA) flux density, and heavily favor highly variable and compact blazars. The sample includes nearly all the most prominent blazars in the northern sky, and is well-suited for statistical analysis and comparison with studies at other wavelengths. Our multi-epoch and stacked-epoch images show 94% of the sample to have apparent one-sided jet morphologies, most likely due to the effects of relativistic beaming. Of the remaining sources, five have two-sided parsec-scale jets, and three are effectively unresolved by the VLBA at 15 GHz, with essentially all of the flux density contained within a few tenths of a milliarcsecond.
{"title":"MOJAVE: Monitoring of Jets in AGN with VLBA Experiments. V. Multi-epoch VLBA Images","authors":"M. Lister, H. Aller, M. Aller, M. Cohen, D. Homan, M. Kadler, K. Kellermann, Y. Y. Kovalev, E. Ros, T. Savolainen, J. Zensus, R. Vermeulen","doi":"10.1088/0004-6256/137/3/3718","DOIUrl":"https://doi.org/10.1088/0004-6256/137/3/3718","url":null,"abstract":"We present images from a long term program (MOJAVE: Monitoring of Jets in AGN with VLBA Experiments) to survey the structure and evolution of parsec-scale jet phenomena associated with bright radio-loud active galaxies in the northern sky. The observations consist of 2424 15 GHz VLBA images of a complete flux-density limited sample of 135 AGN above declination -20 degrees, spanning the period 1994 August to 2007 September. These data were acquired as part of the MOJAVE and 2 cm Survey programs, and from the VLBA archive. The sample selection criteria are based on multi-epoch parsec-scale (VLBA) flux density, and heavily favor highly variable and compact blazars. The sample includes nearly all the most prominent blazars in the northern sky, and is well-suited for statistical analysis and comparison with studies at other wavelengths. Our multi-epoch and stacked-epoch images show 94% of the sample to have apparent one-sided jet morphologies, most likely due to the effects of relativistic beaming. Of the remaining sources, five have two-sided parsec-scale jets, and three are effectively unresolved by the VLBA at 15 GHz, with essentially all of the flux density contained within a few tenths of a milliarcsecond.","PeriodicalId":8453,"journal":{"name":"arXiv: Astrophysics","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2008-12-20","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"83009221","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
{gamma}-ray astronomy has produced for several years now sky maps for low photon statistics, non-negligible background and comparatively poor angular resolution. Quantifying the significance of spatial features remains difficult. Besides, spectrum extraction requires regions with large statistics while maps in energy bands allow only qualitative interpretation. The two main competing mechanisms in the VHE domain are the Inverse-Compton emission from accelerated electrons radiating through synchrotron in the X-ray domain and the interactions between accelerated hadrons and the surrounding medium, leading to the production and subsequent decay of {pi}{sup 0} mesons. The spectrum of the VHE emission from leptons is predicted to steepen with increasing distance from the acceleration zone, owing to synchrotron losses (i.e. cooled population). It would remain approximately constant for hadrons.Ideally, spectro-imaging analysis would have the same spatial scale in the TeV and X-ray domains, to distinguish the local emission mechanisms. More realistically, we investigate here the possibility of improving upon the currently published HESS results by using more sophisticated tools.
{"title":"Morphology and hardness ratio exploitation under limited statistics","authors":"A. Clapson, M. Dyrda, D. Nekrassov, M. Renaud","doi":"10.1063/1.3076767","DOIUrl":"https://doi.org/10.1063/1.3076767","url":null,"abstract":"{gamma}-ray astronomy has produced for several years now sky maps for low photon statistics, non-negligible background and comparatively poor angular resolution. Quantifying the significance of spatial features remains difficult. Besides, spectrum extraction requires regions with large statistics while maps in energy bands allow only qualitative interpretation. The two main competing mechanisms in the VHE domain are the Inverse-Compton emission from accelerated electrons radiating through synchrotron in the X-ray domain and the interactions between accelerated hadrons and the surrounding medium, leading to the production and subsequent decay of {pi}{sup 0} mesons. The spectrum of the VHE emission from leptons is predicted to steepen with increasing distance from the acceleration zone, owing to synchrotron losses (i.e. cooled population). It would remain approximately constant for hadrons.Ideally, spectro-imaging analysis would have the same spatial scale in the TeV and X-ray domains, to distinguish the local emission mechanisms. More realistically, we investigate here the possibility of improving upon the currently published HESS results by using more sophisticated tools.","PeriodicalId":8453,"journal":{"name":"arXiv: Astrophysics","volume":"55 1","pages":"681-684"},"PeriodicalIF":0.0,"publicationDate":"2008-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"89025300","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Pub Date : 2008-12-19DOI: 10.1051/0004-6361:200810912
H. C. Aharonian, E. al.
The rapidly varying (~10 minute timescale) non-thermal X-ray emission observed from Sgr A* implies that particle acceleration is occuring close to the event horizon of the supermassive black hole. The TeV gamma-ray source HESS J1745-290 is coincident with Sgr A* and may be closely related to its X-ray emission. Simultaneous X-ray and TeV observations are required to elucidate the relationship between these objects. We report on joint H.E.S.S./Chandra observations performed in July 2005, during which an X-ray flare was detected. Despite a factor of 9 increase in the X-ray flux of Sgr A*, no evidence is found for an increase in the TeV gamma-ray flux from this region. We find that an increase in the gamma-ray flux of a factor of 2 or greater can be excluded at a confidence level of 99%. This finding disfavours scenarios in which the keV and TeV emission are associated with the same population of accelerated particles and in which the bulk of the gamma-ray emission is produced within ~10^{14} cm (~100 R_S) of the supermassive black hole.
从Sgr A*观测到的快速变化(约10分钟时间尺度)的非热x射线发射表明，粒子加速发生在超大质量黑洞的视界附近。TeV伽玛射线源HESS J1745-290与Sgr A*重合，可能与其x射线发射密切相关。需要同时进行x射线和TeV观测来阐明这些物体之间的关系。我们报告了2005年7月进行的H.E.S.S./钱德拉联合观测，在此期间发现了一个x射线耀斑。尽管Sgr a *的x射线通量增加了9倍，但没有发现该区域的TeV伽马射线通量增加的证据。我们发现，在99%的置信水平上，可以排除γ射线通量增加2倍或更大的因素。这一发现不利于keV和TeV发射与相同的加速粒子群有关的情况，以及大部分伽玛射线发射产生在超大质量黑洞的~10^{14}cm (~100 R_S)范围内。
{"title":"Simultaneous H.E.S.S. and Chandra observations of Sagittarius A* during an X-ray flare","authors":"H. C. Aharonian, E. al.","doi":"10.1051/0004-6361:200810912","DOIUrl":"https://doi.org/10.1051/0004-6361:200810912","url":null,"abstract":"The rapidly varying (~10 minute timescale) non-thermal X-ray emission observed from Sgr A* implies that particle acceleration is occuring close to the event horizon of the supermassive black hole. The TeV gamma-ray source HESS J1745-290 is coincident with Sgr A* and may be closely related to its X-ray emission. Simultaneous X-ray and TeV observations are required to elucidate the relationship between these objects. We report on joint H.E.S.S./Chandra observations performed in July 2005, during which an X-ray flare was detected. Despite a factor of 9 increase in the X-ray flux of Sgr A*, no evidence is found for an increase in the TeV gamma-ray flux from this region. We find that an increase in the gamma-ray flux of a factor of 2 or greater can be excluded at a confidence level of 99%. This finding disfavours scenarios in which the keV and TeV emission are associated with the same population of accelerated particles and in which the bulk of the gamma-ray emission is produced within ~10^{14} cm (~100 R_S) of the supermassive black hole.","PeriodicalId":8453,"journal":{"name":"arXiv: Astrophysics","volume":"55 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2008-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"81113312","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Antarctica offers unique conditions for ground-based observations, such as low sky background in the infrared, improved seeing, and low turbulence and scintillation noise. These properties are particularly beneficial to imaging, precision photometry, and infrared observations. It may be less clear if Antarctica offers equally compelling advantages for spectroscopy, in particular in the optical domain. However, scientific programmes that make use of imaging (or 3D) spectroscopy for selected follow-up studies of IR surveys, long-term monitoring of extended targets and resolved stellar population studies in crowded fields, also benefit from the site conditions at Dome C.
{"title":"Motivations for Imaging Spectroscopy at Dome C","authors":"A. Kelz","doi":"10.1051/eas:0833033","DOIUrl":"https://doi.org/10.1051/eas:0833033","url":null,"abstract":"Antarctica offers unique conditions for ground-based observations, such as low sky background in the infrared, improved seeing, and low turbulence and scintillation noise. These properties are particularly beneficial to imaging, precision photometry, and infrared observations. It may be less clear if Antarctica offers equally compelling advantages for spectroscopy, in particular in the optical domain. However, scientific programmes that make use of imaging (or 3D) spectroscopy for selected follow-up studies of IR surveys, long-term monitoring of extended targets and resolved stellar population studies in crowded fields, also benefit from the site conditions at Dome C.","PeriodicalId":8453,"journal":{"name":"arXiv: Astrophysics","volume":"354 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2008-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"84878412","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
All accretion models of gamma‐ray bursts share a common assumption: accretion power and gravitational binding energy is released and then dissipated locally, with the mass of its origin. This is equivalent to the Shakura‐Sunyaev 1973 (SS73) prescription for the dissipation of accretion power and subsequent conversion into radiate output. Since their seminal paper, broadband observations of quasars and black hole X‐ray binaries insist that the SS73 prescription cannot wholly describe their behavior. In particular, optically thick black hole accretion flows are almost universally accompanied by coronae whose relative power by far exceeds anything seen in studies of stellar chromospheric and coronal activity. In this note, we briefly discuss the possible repercussions of freeing accretion models of GRBs from the SS73 prescription. Our main conclusion is that the efficiency of converting gravitational binding energy into a GRB power can be increased by an order of magnitude or more.
{"title":"On the release of binding energy and accretion power in core collapse‐like environments","authors":"A. Socrates, E. Ramirez-Ruiz","doi":"10.1063/1.3682947","DOIUrl":"https://doi.org/10.1063/1.3682947","url":null,"abstract":"All accretion models of gamma‐ray bursts share a common assumption: accretion power and gravitational binding energy is released and then dissipated locally, with the mass of its origin. This is equivalent to the Shakura‐Sunyaev 1973 (SS73) prescription for the dissipation of accretion power and subsequent conversion into radiate output. Since their seminal paper, broadband observations of quasars and black hole X‐ray binaries insist that the SS73 prescription cannot wholly describe their behavior. In particular, optically thick black hole accretion flows are almost universally accompanied by coronae whose relative power by far exceeds anything seen in studies of stellar chromospheric and coronal activity. In this note, we briefly discuss the possible repercussions of freeing accretion models of GRBs from the SS73 prescription. Our main conclusion is that the efficiency of converting gravitational binding energy into a GRB power can be increased by an order of magnitude or more.","PeriodicalId":8453,"journal":{"name":"arXiv: Astrophysics","volume":"94 1","pages":"474-479"},"PeriodicalIF":0.0,"publicationDate":"2008-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"80328969","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
C. Reylé, P. Delorme, X. Delfosse, T. Forveille, C. Willott, L. Albert, É. Artigau
The Canada‐France Brown Dwarf Survey is a wide field survey for cool brown dwarfs conducted with the MegaCam camera on the CFHT telescope. Our objectives are to find ultracool brown dwarfs and to constrain the field brown dwarf mass function from a large and homogeneous sample of L and T dwarfs. We identify candidates in CFHT/Megacam i’ and z’ images and follow them up with pointed NIR imaging on several telescopes. Our survey has to date found 50 T dwarfs candidates and 170 L or late M dwarf candidates drawn from a larger sample of 1300 candidates with typical ultracool dwarfs i’‐z’ colours, found in 900 square degrees. We currently have completed the NIR follow‐up on a large part of the survey for all candidates from the latest T dwarfs known to the late L color range. This allows us to build on a complete and well defined sample of ultracool dwarfs to investigate the luminosity function of field L and T dwarfs.
加拿大-法国褐矮星调查是一项广泛的低温褐矮星调查，由CFHT望远镜上的MegaCam相机进行。我们的目标是找到超冷褐矮星，并从大量均匀的L和T矮星样本中约束场褐矮星质量函数。我们在CFHT/Megacam i '和z '图像中识别候选者，并在几台望远镜上使用近红外定点成像进行跟踪。迄今为止，我们的调查已经发现了50个T矮星候选者和170个L或晚M矮星候选者，这些候选者是从1300个典型的超冷矮星i '‐z '颜色的候选者中抽取的，发现于900平方度的范围内。目前，我们已经完成了对所有候选者的大部分近红外跟踪调查，从已知的最新T矮星到晚L色范围。这使我们能够建立一个完整的、定义良好的超冷矮星样本来研究场L和T矮星的光度函数。
{"title":"The ultracool field dwarfs luminosity function from the Canada‐France Brown Dwarf Survey","authors":"C. Reylé, P. Delorme, X. Delfosse, T. Forveille, C. Willott, L. Albert, É. Artigau","doi":"10.1063/1.3099171","DOIUrl":"https://doi.org/10.1063/1.3099171","url":null,"abstract":"The Canada‐France Brown Dwarf Survey is a wide field survey for cool brown dwarfs conducted with the MegaCam camera on the CFHT telescope. Our objectives are to find ultracool brown dwarfs and to constrain the field brown dwarf mass function from a large and homogeneous sample of L and T dwarfs. We identify candidates in CFHT/Megacam i’ and z’ images and follow them up with pointed NIR imaging on several telescopes. Our survey has to date found 50 T dwarfs candidates and 170 L or late M dwarf candidates drawn from a larger sample of 1300 candidates with typical ultracool dwarfs i’‐z’ colours, found in 900 square degrees. We currently have completed the NIR follow‐up on a large part of the survey for all candidates from the latest T dwarfs known to the late L color range. This allows us to build on a complete and well defined sample of ultracool dwarfs to investigate the luminosity function of field L and T dwarfs.","PeriodicalId":8453,"journal":{"name":"arXiv: Astrophysics","volume":"32 1","pages":"553-556"},"PeriodicalIF":0.0,"publicationDate":"2008-12-19","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"76164770","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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