Pub Date : 2020-11-06DOI: 10.3847/25C2CFEB.FB466C8B
M. Kelley, H. Hsieh, C. O. Chandler, S. Eggl, T. Holt, L. Jones, M. Jurić, T. Lister, Joachim Moeyens, W. J. Oldroyd, D. Ragozzine, D. Trilling
We outline the challenges faced by the planetary science community in the era of next-generation large-scale astronomical surveys, and highlight needs that must be addressed in order for the community to maximize the quality and quantity of scientific output from archival, existing, and future surveys, while satisfying NASA's and NSF's goals.
{"title":"Community Challenges in the Era of Petabyte-Scale Sky Surveys","authors":"M. Kelley, H. Hsieh, C. O. Chandler, S. Eggl, T. Holt, L. Jones, M. Jurić, T. Lister, Joachim Moeyens, W. J. Oldroyd, D. Ragozzine, D. Trilling","doi":"10.3847/25C2CFEB.FB466C8B","DOIUrl":"https://doi.org/10.3847/25C2CFEB.FB466C8B","url":null,"abstract":"We outline the challenges faced by the planetary science community in the era of next-generation large-scale astronomical surveys, and highlight needs that must be addressed in order for the community to maximize the quality and quantity of scientific output from archival, existing, and future surveys, while satisfying NASA's and NSF's goals.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":"175 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-11-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73165523","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 : 2020-11-06DOI: 10.3847/25C2CFEB.173706D5
A. Rivkin, M. Milazzo, A. Venkatesan, E. Frank, M. Vidaurri, P. Metzger, C. Lewicki
As asteroid mining moves toward reality, the high bar to entering the business may limit participation and increase inequality, reducing or eliminating any benefit gained by marginalized people or developing nations. Consideration of ethical issues is urgently needed, as well as participation in international, not merely multilateral, solutions.
{"title":"Asteroid Resource Utilization: Ethical Concerns and Progress","authors":"A. Rivkin, M. Milazzo, A. Venkatesan, E. Frank, M. Vidaurri, P. Metzger, C. Lewicki","doi":"10.3847/25C2CFEB.173706D5","DOIUrl":"https://doi.org/10.3847/25C2CFEB.173706D5","url":null,"abstract":"As asteroid mining moves toward reality, the high bar to entering the business may limit participation and increase inequality, reducing or eliminating any benefit gained by marginalized people or developing nations. Consideration of ethical issues is urgently needed, as well as participation in international, not merely multilateral, solutions.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":"60 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-11-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"72723596","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 : 2020-11-05DOI: 10.1103/physrevd.103.023004
S. Rowlinson, A. Dmitriev, A. Jones, Teng Zhang, A. Freise
The optical design of the Einstein Telescope (ET) is based on a dual-recycled Michelson interferometer with Fabry-Perot cavities in the arms. ET will be constructed in a new infrastructure, allowing us to consider different technical implementations beyond the constraints of the current facilities. In this paper we investigate the feasibility of using beam-expander telescopes in the interferometer arms. We provide an example implementation that matches the optical layout as presented in the ET design update 2020. We further show that the beam-expander telescopes can be tuned to compensate for mode mismatches between the arm cavities and the rest of the interferometer.
{"title":"Feasibility study of beam-expanding telescopes in the interferometer arms for the Einstein Telescope","authors":"S. Rowlinson, A. Dmitriev, A. Jones, Teng Zhang, A. Freise","doi":"10.1103/physrevd.103.023004","DOIUrl":"https://doi.org/10.1103/physrevd.103.023004","url":null,"abstract":"The optical design of the Einstein Telescope (ET) is based on a dual-recycled Michelson interferometer with Fabry-Perot cavities in the arms. ET will be constructed in a new infrastructure, allowing us to consider different technical implementations beyond the constraints of the current facilities. In this paper we investigate the feasibility of using beam-expander telescopes in the interferometer arms. We provide an example implementation that matches the optical layout as presented in the ET design update 2020. We further show that the beam-expander telescopes can be tuned to compensate for mode mismatches between the arm cavities and the rest of the interferometer.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":"6 4","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-11-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"72597748","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 : 2020-11-03DOI: 10.1051/0004-6361/201936291
U. Heiter, K. Lind, M. Bergemann, M. Asplund, vSarunas Mikolaitis, P. Barklem, T. Masseron, P. Laverny, L. Magrini, B. Edvardsson, Henrik Jonsson, Juliet C. Pickering, N. Ryde, Amelia Bayo Ar'an, T. Bensby, A. Casey, S. Feltzing, P. Jofr'e, A. Korn, E. Pancino, F. Damiani, A. Lanzafame, C. Lardo, L. Monaco, L. Morbidelli, R. Smiljanic, C. Worley, S. Zaggia, S. Randich, Gerard F. Gilmore
We describe the atomic and molecular data that were used for the abundance analyses of FGK-type stars carried out within the Gaia-ESO Survey. We present an unprecedented effort to create a homogeneous line list, which was used by several abundance analysis groups to calculate synthetic spectra and equivalent widths. The atomic data are accompanied by quality indicators and detailed references to the sources. The atomic and molecular data are made publicly available in electronic form. In general experimental transition probabilities were preferred but theoretical values were also used. Astrophysical gf-values were avoided due to the model-dependence of such a procedure. For elements whose lines are significantly affected by hyperfine structure or isotopic splitting a concerted effort has been made to collate the necessary data for the individual line components. We also performed a detailed investigation of available data for line broadening due to collisions with neutral hydrogen atoms. Synthetic spectra calculated for the Sun and Arcturus were used to assess the blending properties of the lines. Among a subset of over 1300 lines of 35 elements in the wavelength ranges from 475 nm to 685 nm and from 850 nm to 895 nm we identified about 200 lines of 24 species which have accurate gf-values and are free of blends in the spectra of the Sun and Arcturus. For the broadening due to collisions with neutral hydrogen we recommend data based on Anstee-Barklem-O'Mara theory, where available, and to avoid lines of neutral species otherwise. Theoretical broadening data by R.L. Kurucz should be used for Sc II, Ti II, and Y II lines. For ionised rare-earth species the Uns"old approximation with an enhancement factor of 1.5 for the line width can be used. Desirable improvements in atomic data were identified for a number of species, including Al I, S I, Cr II, Na I, Si I, Ca II, and Ni I.
我们描述了用于Gaia-ESO调查中进行的fgk型恒星丰度分析的原子和分子数据。我们提出了一个前所未有的努力来创建一个均匀线列表，它被几个丰度分析小组用来计算合成光谱和等效宽度。原子数据附有质量指标和对来源的详细参考。原子和分子数据以电子形式公开提供。一般情况下，首选实验跃迁概率，但也使用理论值。由于这种程序依赖于模型，因此避免了天体物理gf值。对于其谱线受到超精细结构或同位素分裂的显著影响的元素，已作出协调一致的努力来整理各个谱线组分的必要数据。我们还对与中性氢原子碰撞引起的谱线展宽进行了详细的研究。计算太阳和大角星的合成光谱用于评估谱线的混合特性。在波长范围从475 nm到685 nm和850 nm到895 nm的1300多行35种元素的子集中，我们确定了24种大约200行具有准确的gf值，并且在太阳和大角星的光谱中没有混合。对于与中性氢碰撞导致的加宽，我们推荐基于Anstee-Barklem-O'Mara理论的数据，如果有的话，并且避免中性物质的谱线。R.L. Kurucz的理论展宽数据应用于Sc II、Ti II和Y II系。对于离子化稀土，可以使用线宽增强因子为1.5的旧近似。原子数据的理想改进被确定为许多物种，包括Al I, S I, Cr II, Na I, Si I, Ca II和Ni I。
{"title":"Atomic data for the Gaia-ESO Survey","authors":"U. Heiter, K. Lind, M. Bergemann, M. Asplund, vSarunas Mikolaitis, P. Barklem, T. Masseron, P. Laverny, L. Magrini, B. Edvardsson, Henrik Jonsson, Juliet C. Pickering, N. Ryde, Amelia Bayo Ar'an, T. Bensby, A. Casey, S. Feltzing, P. Jofr'e, A. Korn, E. Pancino, F. Damiani, A. Lanzafame, C. Lardo, L. Monaco, L. Morbidelli, R. Smiljanic, C. Worley, S. Zaggia, S. Randich, Gerard F. Gilmore","doi":"10.1051/0004-6361/201936291","DOIUrl":"https://doi.org/10.1051/0004-6361/201936291","url":null,"abstract":"We describe the atomic and molecular data that were used for the abundance analyses of FGK-type stars carried out within the Gaia-ESO Survey. We present an unprecedented effort to create a homogeneous line list, which was used by several abundance analysis groups to calculate synthetic spectra and equivalent widths. The atomic data are accompanied by quality indicators and detailed references to the sources. The atomic and molecular data are made publicly available in electronic form. In general experimental transition probabilities were preferred but theoretical values were also used. Astrophysical gf-values were avoided due to the model-dependence of such a procedure. For elements whose lines are significantly affected by hyperfine structure or isotopic splitting a concerted effort has been made to collate the necessary data for the individual line components. We also performed a detailed investigation of available data for line broadening due to collisions with neutral hydrogen atoms. Synthetic spectra calculated for the Sun and Arcturus were used to assess the blending properties of the lines. Among a subset of over 1300 lines of 35 elements in the wavelength ranges from 475 nm to 685 nm and from 850 nm to 895 nm we identified about 200 lines of 24 species which have accurate gf-values and are free of blends in the spectra of the Sun and Arcturus. For the broadening due to collisions with neutral hydrogen we recommend data based on Anstee-Barklem-O'Mara theory, where available, and to avoid lines of neutral species otherwise. Theoretical broadening data by R.L. Kurucz should be used for Sc II, Ti II, and Y II lines. For ionised rare-earth species the Uns\"old approximation with an enhancement factor of 1.5 for the line width can be used. Desirable improvements in atomic data were identified for a number of species, including Al I, S I, Cr II, Na I, Si I, Ca II, and Ni I.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-11-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"81025029","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 : 2020-11-02DOI: 10.1103/PHYSREVD.103.022003
C. Blair, Y. Levin, E. Thrane
Thermal distortion of test masses, as well as thermal drift of their vibrational mode frequencies, present a major challenge for operation of the Advanced LIGO and Advanced VIRGO interferometers, reducing optical efficiency, which limits sensitivity and potentially causing instabilities which reduce duty-cycle. In this paper, we demonstrate that test-mass vibrational mode frequency data can be used to overcome some of these difficulties. First, we derive a general expression for the change in a mode frequency as a function of temperature distribution inside the test mass. Then we show how the mode frequency dependence on temperature distribution can be used to identify the wavefunction of observed vibrational modes. We then show how monitoring the frequencies of multiple vibrational modes allows the temperature distribution inside the test mass to be strongly constrained. Finally, we demonstrate using simulations, the potential to improve the thermal model of the test mass, providing independent and improved estimates of important parameters such as the coating absorption coefficient and the location of point absorbers.
{"title":"Constraining temperature distribution inside LIGO test masses from frequencies of their vibrational modes","authors":"C. Blair, Y. Levin, E. Thrane","doi":"10.1103/PHYSREVD.103.022003","DOIUrl":"https://doi.org/10.1103/PHYSREVD.103.022003","url":null,"abstract":"Thermal distortion of test masses, as well as thermal drift of their vibrational mode frequencies, present a major challenge for operation of the Advanced LIGO and Advanced VIRGO interferometers, reducing optical efficiency, which limits sensitivity and potentially causing instabilities which reduce duty-cycle. In this paper, we demonstrate that test-mass vibrational mode frequency data can be used to overcome some of these difficulties. First, we derive a general expression for the change in a mode frequency as a function of temperature distribution inside the test mass. Then we show how the mode frequency dependence on temperature distribution can be used to identify the wavefunction of observed vibrational modes. We then show how monitoring the frequencies of multiple vibrational modes allows the temperature distribution inside the test mass to be strongly constrained. Finally, we demonstrate using simulations, the potential to improve the thermal model of the test mass, providing independent and improved estimates of important parameters such as the coating absorption coefficient and the location of point absorbers.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":"2017 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-11-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"77682991","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 : 2020-11-02DOI: 10.1142/s2251171720500178
B. Donovan, R. McEntaffer, C. DeRoo, J. Tutt, F. Gris'e, Chad M. Eichfel, Oren Z. Gall, V. Burwitz, G. Hartner, C. Pelliciari, Marlis-Madeleine La Caria
The soft X-ray grating spectrometer on board the Off-plane Grating Rocket Experiment (OGRE) hopes to achieve the highest resolution soft X-ray spectrum of an astrophysical object when it is launched via suborbital rocket. Paramount to the success of the spectrometer are the performance of the $>250$ reflection gratings populating its reflection grating assembly. To test current grating fabrication capabilities, a grating prototype for the payload was fabricated via electron-beam lithography at The Pennsylvania State University's Materials Research Institute and was subsequently tested for performance at Max Planck Institute for Extraterrestrial Physics' PANTER X-ray Test Facility. Bayesian modeling of the resulting data via Markov chain Monte Carlo (MCMC) sampling indicated that the grating achieved the OGRE single-grating resolution requirement of $R_{g}(lambda/Deltalambda)>4500$ at the 94% confidence level. The resulting $R_g$ posterior probability distribution suggests that this confidence level is likely a conservative estimate though, since only a finite $R_g$ parameter space was sampled and the model could not constrain the upper bound of $R_g$ to less than infinity. Raytrace simulations of the system found that the observed data can be reproduced with a grating performing at $R_g=infty$. It is therefore postulated that the behavior of the obtained $R_g$ posterior probability distribution can be explained by a finite measurement limit of the system and not a finite limit on $R_g$. Implications of these results and improvements to the test setup are discussed.
离机光栅火箭实验(OGRE)机载软x射线光栅光谱仪希望通过亚轨道火箭发射获得天体物理物体的最高分辨率软x射线光谱。对于光谱仪的成功至关重要的是其反射光栅组件中$>250$反射光栅的性能。为了测试当前的光栅制造能力，宾夕法尼亚州立大学材料研究所通过电子束光刻技术制造了有效载荷的光栅原型，随后在马克斯普朗克地外物理研究所的PANTER x射线测试设施进行了性能测试。通过马尔可夫链蒙特卡罗(MCMC)采样对所得数据进行贝叶斯建模，表明该光栅在94时达到了OGRE单光栅分辨率$R_{g}(lambda/Deltalambda)>4500$的要求% confidence level. The resulting $R_g$ posterior probability distribution suggests that this confidence level is likely a conservative estimate though, since only a finite $R_g$ parameter space was sampled and the model could not constrain the upper bound of $R_g$ to less than infinity. Raytrace simulations of the system found that the observed data can be reproduced with a grating performing at $R_g=infty$. It is therefore postulated that the behavior of the obtained $R_g$ posterior probability distribution can be explained by a finite measurement limit of the system and not a finite limit on $R_g$. Implications of these results and improvements to the test setup are discussed.
{"title":"Performance Testing of a Large-Format X-ray Reflection Grating Prototype for a Suborbital Rocket Payload","authors":"B. Donovan, R. McEntaffer, C. DeRoo, J. Tutt, F. Gris'e, Chad M. Eichfel, Oren Z. Gall, V. Burwitz, G. Hartner, C. Pelliciari, Marlis-Madeleine La Caria","doi":"10.1142/s2251171720500178","DOIUrl":"https://doi.org/10.1142/s2251171720500178","url":null,"abstract":"The soft X-ray grating spectrometer on board the Off-plane Grating Rocket Experiment (OGRE) hopes to achieve the highest resolution soft X-ray spectrum of an astrophysical object when it is launched via suborbital rocket. Paramount to the success of the spectrometer are the performance of the $>250$ reflection gratings populating its reflection grating assembly. To test current grating fabrication capabilities, a grating prototype for the payload was fabricated via electron-beam lithography at The Pennsylvania State University's Materials Research Institute and was subsequently tested for performance at Max Planck Institute for Extraterrestrial Physics' PANTER X-ray Test Facility. Bayesian modeling of the resulting data via Markov chain Monte Carlo (MCMC) sampling indicated that the grating achieved the OGRE single-grating resolution requirement of $R_{g}(lambda/Deltalambda)>4500$ at the 94% confidence level. The resulting $R_g$ posterior probability distribution suggests that this confidence level is likely a conservative estimate though, since only a finite $R_g$ parameter space was sampled and the model could not constrain the upper bound of $R_g$ to less than infinity. Raytrace simulations of the system found that the observed data can be reproduced with a grating performing at $R_g=infty$. It is therefore postulated that the behavior of the obtained $R_g$ posterior probability distribution can be explained by a finite measurement limit of the system and not a finite limit on $R_g$. Implications of these results and improvements to the test setup are discussed.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":"43 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-11-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"86852500","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}
H. Spreeuw, S. Yatawatta, B. V. Werkhoven, F. Diblen
As astronomical instruments become more sensitive, the requirements for the calibration software become more stringent; without accurate calibration solutions, thermal noise levels in images will not be reached and the scientific output of the instrument is degraded. Calibration requires bright sources with known properties, in particular with respect to their brightnesses as a function of frequency. However, for modern radio telescopes with a huge field of view, a single calibration source does not suffice; instead a sky model with tens of thousands of sources is needed. In this work, we investigate the compute load for such complicated sky models, with up to 50,000 sources, for the SAGECal calibration package. We have chosen half of the sources in these models to be point sources and half of them extended, which we represent by Gaussian profiles.
{"title":"SAGECal Performance With Large Sky Models","authors":"H. Spreeuw, S. Yatawatta, B. V. Werkhoven, F. Diblen","doi":"10.46620/20-0026","DOIUrl":"https://doi.org/10.46620/20-0026","url":null,"abstract":"As astronomical instruments become more sensitive, the requirements for the calibration software become more stringent; without accurate calibration solutions, thermal noise levels in images will not be reached and the scientific output of the instrument is degraded. Calibration requires bright sources with known properties, in particular with respect to their brightnesses as a function of frequency. However, for modern radio telescopes with a huge field of view, a single calibration source does not suffice; instead a sky model with tens of thousands of sources is needed. In this work, we investigate the compute load for such complicated sky models, with up to 50,000 sources, for the SAGECal calibration package. We have chosen half of the sources in these models to be point sources and half of them extended, which we represent by Gaussian profiles.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":"32 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-10-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"81760796","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. Amon, K. Bechtol, A. Connolly, S. Digel, A. Drlica-Wagner, E. Gawiser, M. Jarvis, S. Jha, A. von der Linden, M. Moniez, G. Narayan, N. Regnault, I. Sevilla-Noarbe, S. Schmidt, S. Suyu, C. Walter
The commissioning team for the Vera C. Rubin observatory is planning a set of engineering and science verification observations with the Legacy Survey of Space and Time (LSST) commissioning camera and then the Rubin Observatory LSST Camera. The time frame for these observations is not yet fixed, and the commissioning team will have flexibility in selecting fields to observe. In this document, the Dark Energy Science Collaboration (DESC) Commissioning Working Group presents a prioritized list of target fields appropriate for testing various aspects of DESC-relevant science performance, grouped by season for visibility from Rubin Observatory at Cerro Pachon. Our recommended fields include Deep-Drilling fields (DDFs) to full LSST depth for photo-$z$ and shape calibration purposes, HST imaging fields to full depth for deblending studies, and an $sim$200 square degree area to 1-year depth in several filters for higher-level validation of wide-area science cases for DESC. We also anticipate that commissioning observations will be needed for template building for transient science over a broad RA range. We include detailed descriptions of our recommended fields along with associated references. We are optimistic that this document will continue to be useful during LSST operations, as it provides a comprehensive list of overlapping data-sets and the references describing them.
Vera C. Rubin天文台的调试团队正在计划用遗留时空调查(LSST)调试相机和鲁宾天文台LSST相机进行一系列工程和科学验证观测。这些观察的时间框架尚未确定，委托小组在选择观察领域方面将具有灵活性。在这份文件中，暗能量科学合作(DESC)调试工作组提出了一个优先级列表，适合测试DESC相关科学性能的各个方面，按季节分组，从Cerro Pachon的鲁宾天文台可见。我们推荐的领域包括深度钻探领域(ddf)至全LSST深度，用于照片- z -$和形状校准目的，HST成像领域至全深度，用于解混研究，以及几个过滤器的200平方度区域至1年深度，用于DESC广域科学案例的更高级别验证。我们还预计，在广泛的RA范围内，将需要调试观测来构建瞬态科学的模板。我们包括我们推荐的字段的详细描述以及相关的参考资料。我们乐观地认为，该文件将在LSST操作期间继续有用，因为它提供了重叠数据集的综合列表和描述它们的参考文献。
{"title":"Recommended Target Fields for Commissioning the Vera C. Rubin Observatory","authors":"A. Amon, K. Bechtol, A. Connolly, S. Digel, A. Drlica-Wagner, E. Gawiser, M. Jarvis, S. Jha, A. von der Linden, M. Moniez, G. Narayan, N. Regnault, I. Sevilla-Noarbe, S. Schmidt, S. Suyu, C. Walter","doi":"10.2172/1833575","DOIUrl":"https://doi.org/10.2172/1833575","url":null,"abstract":"The commissioning team for the Vera C. Rubin observatory is planning a set of engineering and science verification observations with the Legacy Survey of Space and Time (LSST) commissioning camera and then the Rubin Observatory LSST Camera. The time frame for these observations is not yet fixed, and the commissioning team will have flexibility in selecting fields to observe. In this document, the Dark Energy Science Collaboration (DESC) Commissioning Working Group presents a prioritized list of target fields appropriate for testing various aspects of DESC-relevant science performance, grouped by season for visibility from Rubin Observatory at Cerro Pachon. Our recommended fields include Deep-Drilling fields (DDFs) to full LSST depth for photo-$z$ and shape calibration purposes, HST imaging fields to full depth for deblending studies, and an $sim$200 square degree area to 1-year depth in several filters for higher-level validation of wide-area science cases for DESC. We also anticipate that commissioning observations will be needed for template building for transient science over a broad RA range. We include detailed descriptions of our recommended fields along with associated references. We are optimistic that this document will continue to be useful during LSST operations, as it provides a comprehensive list of overlapping data-sets and the references describing them.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":"10 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-10-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"74523256","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}
In this work we compute a reasonably comprehensive set of tables for current and next generation survey facility filter conversions. Almost all useful transforms are included with the ProSpect software package described in Robotham et al (2020). Users are free to provide their own filters and compute their own transforms, where the included package examples outline the approach. This arXiv document will be relatively frequently updated, so people are encouraged to get in touch with their suggestions for additional utility (i.e. new filter sets).
{"title":"Current and Next Generation Survey Filter Conversions with ProSpect","authors":"A. Robotham","doi":"10.7910/DVN/ZPW9OQ","DOIUrl":"https://doi.org/10.7910/DVN/ZPW9OQ","url":null,"abstract":"In this work we compute a reasonably comprehensive set of tables for current and next generation survey facility filter conversions. Almost all useful transforms are included with the ProSpect software package described in Robotham et al (2020). Users are free to provide their own filters and compute their own transforms, where the included package examples outline the approach. This arXiv document will be relatively frequently updated, so people are encouraged to get in touch with their suggestions for additional utility (i.e. new filter sets).","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":"20 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-10-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"73619064","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}
T. Nakamori, Yuga Ouchi, Risa Ogihara, T. Terasawa, Yuhei Kato, S. Shibata
We have developed a sensor system based on an optical photon-counting imager with high timing resolution, aiming for highly time-variable astronomical phenomena. The detector is a monolithic Geiger-mode avalanche photodiode array customized in a Multi-Pixel Photon Counter with a response time on the order of nanoseconds. This paper evaluates the basic performance of the sensor and confirms the gain linearity, uniformity, and low dark count. We demonstrate the system's ability to detect the period of a flashing LED, using a data acquisition system developed to obtain the light curve with a time bin of 100 microseconds. The Crab pulsar was observed using a 35-cm telescope without cooling, and the equipment detected optical pulses with a period consistent with the data from the radio ephemeris. Although improvements to the system will be necessary for more reliability, the system has been proven to be a promising device for exploring the time-domain optical astronomy.
{"title":"Development of an optical photon-counting imager with a monolithic Geiger Avalanche Photodiode array","authors":"T. Nakamori, Yuga Ouchi, Risa Ogihara, T. Terasawa, Yuhei Kato, S. Shibata","doi":"10.1093/pasj/psaa106","DOIUrl":"https://doi.org/10.1093/pasj/psaa106","url":null,"abstract":"We have developed a sensor system based on an optical photon-counting imager with high timing resolution, aiming for highly time-variable astronomical phenomena. The detector is a monolithic Geiger-mode avalanche photodiode array customized in a Multi-Pixel Photon Counter with a response time on the order of nanoseconds. This paper evaluates the basic performance of the sensor and confirms the gain linearity, uniformity, and low dark count. We demonstrate the system's ability to detect the period of a flashing LED, using a data acquisition system developed to obtain the light curve with a time bin of 100 microseconds. The Crab pulsar was observed using a 35-cm telescope without cooling, and the equipment detected optical pulses with a period consistent with the data from the radio ephemeris. Although improvements to the system will be necessary for more reliability, the system has been proven to be a promising device for exploring the time-domain optical astronomy.","PeriodicalId":8459,"journal":{"name":"arXiv: Instrumentation and Methods for Astrophysics","volume":"1 1","pages":""},"PeriodicalIF":0.0,"publicationDate":"2020-10-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"90880856","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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