Plane Survey(平面测量)研究综述
Plane Survey 平面测量 - The GHRSS survey is an off-Galactic-plane survey at 322 MHz in a region of the sky (declination range -40 degrees to -54 degrees) complementary to other ongoing low-frequency surveys. [1]GHRSS 调查是在天空区域（偏角范围 -40 度至 -54 度）的 322 MHz 的离银河平面调查，是对其他正在进行的低频调查的补充。 [1]
Galactic Plane Survey 银河平面调查
We present the goals, strategy and first results of the high-cadence Galactic plane survey using the Zwicky Transient Facility (ZTF). [1] Galactic Plane Survey (HGPS) revealed 78 TeV sources among which 47 are not clearly associated with a known object. [2] We report on the implications of TeV Pulsar Wind Nebulae observed by the HESS Galactic Plane Survey in the 1-100 TeV energy range for the interpretation of Fermi-LAT data. [3] Galactic plane survey data, applying an analysis technique comparable between H. [4] Galactic Plane Survey (HGPS) catalogue. [5] For a preliminary validation, a comparison with the 843 MHz Molonglo Galactic Plane Survey is presented. [6] The Cygnus X complex is covered by the Global View of Star Formation in the Milky Way (GLOSTAR) survey, an unbiased radio-wavelength Galactic plane survey, in 4–8 GHz continuum radiation and several spectral lines. [7] sources observed in their Galactic Plane Survey. [8] We present a new catalog of rotation measures derived from the Canadian Galactic Plane Survey, covering a large region of the Galactic plane spanning 52° < l < 192°, −3° < b < 5°, along with northern and southern latitude extensions around l ≈ 105°. [9] Among them, the PWN HESS J1837−069 was detected earlier by the HESS observatory during its first galactic plane survey. [10] 5 arcsecond, similar to complementary near-IR and mid-IR galactic plane surveys. [11] Galactic plane survey, a numerical approach has been taken to develop a model of the population of Galactic VHE γ-ray sources, which is shown to account accurately for the observational bias. [12] Infrared archival data were obtained from the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE), the Multi-band Imaging Photometer Survey of the Galaxy (MIPSGAL), and the Herschel Infrared Galactic Plane Survey (Hi-GAL). [13] Equipped for observations at 1420 and 408 MHz, the ST completed the Canadian Galactic Plane Survey, providing pioneering measurements of arcminute-scale structure in HI emission and self-absorption and of the diffuse polarized emission, using a fine grid of Rotation Measures to chart the large-scale Galactic magnetic field, and advancing the knowledge of the Galactic rotation curve. [14] The possibility of conducting a Galactic plane survey at energies above 5 keV with the ART-XC telescope onboard the Spectrum-Röntgen-Gamma (SRG) observatory during the satellite’s flight to the Lagrange point L2 is considered. [15] However, this decomposition requires full automation lest it becomes prohibitive for large datasets, such as Galactic plane surveys. [16] The Milky Way Project (MWP), a citizen science initiative on the Zooniverse platform, presents internet users with infrared (IR) images from Spitzer Space Telescope Galactic plane surveys. [17] We discover previously undetected signposts of low-luminosity star formation from CO (2-1) and SiO (5-4) bipolar outflows and other signatures towards 11 out of 12 clumps, showing that current MIR/FIR Galactic Plane surveys are incomplete to low- and intermediate-mass protostars ($\lesssim 50\, L_\odot$). [18] We present a morphological and physical analysis of a Giant Molecular Cloud (GMC) using the carbon monoxide isotopologues ($^{12}$CO, $^{13}$CO, C$^{18}$O $^{3}P_{2}\rightarrow$ $^{3}P_{1}$) survey of the Galactic Plane (Mopra CO Southern Galactic Plane Survey), supplemented with neutral carbon maps from the HEAT telescope in Antarctica. [19] We then consider a sample of sources associated to PWNe and detected in the HESS Galactic plane survey and in the second HAWC catalog. [20] The latest generation of high-angular-resolution unbiased Galactic plane surveys in molecular-gas tracers are enabling the interiors of molecular clouds to be studied across a range of environments. [21] We publish all OH and RRL data from the C-configuration observations, and a new H I dataset combining VLA C+D+GBT (VLA D-configuration and GBT data are from the VLA Galactic Plane Survey) for the whole survey. [22] We investigate the interstellar medium towards seven TeV gamma-ray sources thought to be pulsar wind nebulae using Mopra molecular line observations at 7 mm [CS(1–0), SiO(1–0, v = 0)], Nanten CO(1–0) data and the Southern Galactic Plane Survey/GASS Hi survey. [23] We used polarisation data from the Canadian Galactic Plane Survey (CGPS), observed near 1420 MHz with the Dominion Radio Astrophysical Observatory (DRAO) Synthesis Telescope. [24] The infrared archival data come from Galactic Legacy Infrared Midplane Survey Extraordinaire (GLIMPSE), Wide-field Infrared Survey Explorer (WISE) and Herschel InfraRed Galactic Plane Survey (HiGAL). [25] Applying the synergies of synchrotron diagnostic gradients to the archive data from the Canadian Galactic Plane Survey, we find that multifarious diagnostic techniques make consistent predictions for the Galactic magnetic field directions. [26] We identify their constituent clumps using thermal dust emission, as observed by the Herschel infrared GALactic plane survey (Hi-GAL). [27] Galactic Plane Survey (hgps, [1]) from the Southern Hemisphere, but also magic and veritas contributed to this population with the discoveries of 3c 58 and ct1 towards the outer part of the Milky Way [2, 3]. [28] For each SNR the SHALON observation results are given with its spectral energy distribution compared with other experimental data and images by SHALON together with data from X-ray by Chandra and radio-data by Canadian Galactic Plane Survey DRAO (CGPS). [29] The Canadian Galactic Plane Survey identified a wealth of small-scale structure in H I emission as well as self-absorption and in the structure of polarized emission. [30] Lower limits on the energy cutoff for unidentified γ-ray sources detected in the High Energy Stereoscopic System (HESS) Galactic plane survey were derived. [31] A number of developments have been done driven by the analysis of the SCORPIO map and in view of the future ASKAP Galactic Plane survey. [32] Even though larger than our target sensitivity of 2 mJy, the current sensitivity already allows the identification of a new population of cold, compact sources that remained undetected in any (sub-)mm Galactic plane survey so far. [33] We investigated the chemical evolution of HC3N in six dense molecular clouds, using archival available data from the Herschel infrared Galactic Plane Survey (Hi-GAL) and the Millimeter Astronomy Legacy Team Survey at 90 GHz (MALT90). [34] The public time contains two surveys: a 3-day cadence for the Northern Sky Survey and a 1-day cadence for the Galactic Plane Survey. [35] MAXI J1621-501 is the first Swift/XRT Deep Galactic Plane Survey transient that was followed up with a multitude of space missions (NuSTAR, Swift, Chandra, NICER, INTEGRAL, and MAXI) and ground-based observatories (Gemini, IRSF, and ATCA). [36] The Canadian Galactic Plane Survey 12CO line data (beam size ~100". [37] We search for far-infrared (FIR) counterparts of known supernova remnants (SNRs) in the Galactic plane (10° < ∣l∣ < 60°) at 70 – 500 μm using the Herschel Infrared Galactic Plane Survey (Hi-GAL). [38]我们介绍了使用 Zwicky 瞬态设施 (ZTF) 进行的高节奏银河平面调查的目标、策略和初步结果。 [1] 银河平面调查 (HGPS) 揭示了 78 个 TeV 源，其中 47 个与已知物体没有明确关联。 [2] 我们报告了 HESS 银河平面调查在 1-100 TeV 能量范围内观测到的 TeV 脉冲星风星云对解释 Fermi-LAT 数据的影响。 [3] 银河平面调查数据，采用 H. [4] 银河平面测量 (HGPS) 目录。 [5] 为了进行初步验证，我们提供了与 843 MHz Molonglo 银河平面测量的比较。 [6] 天鹅座 X 复合体被银河系恒星形成全球视图 (GLOSTAR) 调查所覆盖，这是一项无偏无线电波长银河平面调查，在 4-8 GHz 连续辐射和几条谱线中进行。 [7] 在他们的银河平面调查中观察到的来源。 [8] 我们提出了一个新的旋转测量目录，该目录源自加拿大银河平面调查，涵盖了跨越 52° < l < 192°、-3° < b < 5° 的银河平面的大片区域，以及周围的北纬和南纬延伸。 l ≈ 105°。 [9] 其中，PWN HESS J1837-069 是由 HESS 天文台在首次银河平面巡天时较早发现的。 [10] 5 角秒，类似于互补的近红外和中红外银河平面测量。 [11] 银河平面调查，采用数值方法开发了银河 VHE γ 射线源种群模型，该模型被证明可以准确地解释观测偏差。 [12] 红外档案数据来自银河传统红外中平面巡天 (GLIMPSE)、银河多波段成像光度计巡天 (MIPSGAL) 和赫歇尔红外银河平面巡天 (Hi-GAL)。 [13] ST 配备了 1420 和 408 MHz 的观测设备，完成了加拿大银河平面测量，提供了 HI 发射和自吸收的弧分尺度结构以及漫极化发射的开创性测量，使用精细的旋转测量网格来绘制大尺度银河磁场，推进银河自转曲线的认识。 [14] 考虑在卫星飞往拉格朗日点 L2 期间，使用 Spectrum-Röntgen-Gamma (SRG) 天文台上的 ART-XC 望远镜以高于 5 keV 的能量进行银河平面测量的可能性。 [15] 但是，这种分解需要完全自动化，以免它对大型数据集（例如银河平面调查）变得望而却步。 [16] 银河计划 (MWP) 是 Zooniverse 平台上的一项公民科学计划，它向互联网用户展示来自斯皮策太空望远镜银河平面调查的红外 (IR) 图像。 [17] 我们发现了以前未被发现的低光度恒星形成路标，来自 CO (2-1) 和 SiO (5-4) 双极流出和其他特征朝向 12 个团块中的 11 个，表明当前的 MIR/FIR 银河平面调查不完整到低- 和中等质量的原恒星（$\lesssim 50\, L_\odot$）。 [18] 我们使用一氧化碳同位素体（$^{12}$CO, $^{13}$CO, C$^{18}$O $^{3} P_{2}\rightarrow$ $^{3}P_{1}$) 银河平面调查（Mopra CO 南部银河平面调查），并辅以来自南极洲 HEAT 望远镜的中性碳图。 [19] 然后，我们考虑在 HESS 银河平面调查和第二个 HAWC 目录中检测到的与 PWNe 相关的源样本。 [20] 分子气体示踪剂中最新一代的高角分辨率无偏银河平面调查使分子云的内部能够在一系列环境中进行研究。 [21] 我们发布了来自 C 配置观测的所有 OH 和 RRL 数据，以及一个新的 HI 数据集，该数据集结合了 VLA C+D+GBT（VLA D 配置和 GBT 数据来自 VLA 银河平面调查）用于整个调查。 [22] 我们使用 Mopra 分子线观测 7 mm [CS(1-0), SiO(1-0, v = 0)], Nanten CO(1 –0) 数据和南部银河平面调查/GASS Hi 调查。 [23] 我们使用了来自加拿大银河平面测量 (CGPS) 的极化数据，这些数据是用 Dominion Radio Astrophysical Observatory (DRAO) 合成望远镜在 1420 MHz 附近观测到的。 [24] 红外档案数据来自银河传统红外中平面巡天 (GLIMPSE)、广域红外巡天探测器 (WISE) 和赫歇尔红外银河平面巡天 (HiGAL)。 [25] 将同步加速器诊断梯度的协同作用应用于加拿大银河平面调查的档案数据，我们发现多种诊断技术对银河磁场方向做出一致的预测。 [26] 正如 Herschel 红外银河平面调查 (Hi-GAL) 所观察到的，我们使用热尘埃发射来识别它们的组成团块。 [27] 来自南半球的银河平面调查 (hgps, [1])，还有魔法和真理对银河系外围的 3c 58 和 ct1 的发现做出了贡献 [2, 3]。 [28] 对于每个信噪比，SHALON 观测结果都给出了其光谱能量分布，并与其他实验数据和 SHALON 图像以及 Chandra 的 X 射线数据和加拿大银河平面测量 DRAO (CGPS) 的无线电数据进行了比较。 [29] 加拿大银河平面调查在 H I 发射以及自吸收和极化发射结构中发现了丰富的小尺度结构。 [30] 导出了在高能立体系统 (HESS) 银河平面调查中检测到的未识别 γ 射线源的能量截止下限。 [31] 对 SCORPIO 地图的分析以及未来的 ASKAP 银河平面调查已经推动了许多发展。 [32] 尽管大于我们 2 mJy 的目标灵敏度，但目前的灵敏度已经允许识别出迄今为止在任何（亚）毫米银河平面调查中仍未发现的新的冷致密源群体。 [33] 我们利用赫歇尔红外银河平面巡天 (Hi-GAL) 和 90 GHz 毫米天文学遗产团队巡天 (MALT90) 的存档可用数据，研究了六种致密分子云中 HC3N 的化学演化。 [34] 公共时间包含两个调查：北方天空调查的 3 天节奏和银河平面调查的 1 天节奏。 [35] MAXI J1621-501 是第一个 Swift/XRT 深银河平面测量瞬变，随后进行了大量太空任务（NuSTAR、Swift、Chandra、NICER、INTEGRAL 和 MAXI）和地面观测站（Gemini、IRSF 和ATCA)。 [36] 加拿大银河平面调查 12CO 线数据（光束大小 ~100"。 [37] 我们使用赫歇尔红外银河平面调查 (Hi-GAL) 在 70 – 500 μm 的银河平面 (10° < ∣l∣ < 60°) 中搜索已知超新星遗迹 (SNR) 的远红外 (FIR) 对应物。 [38]
plane survey extraordinaire
Infrared archival data were obtained from the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE), the Multi-band Imaging Photometer Survey of the Galaxy (MIPSGAL), and the Herschel Infrared Galactic Plane Survey (Hi-GAL). [1] The new extinction map features a maximum bin size of 1', and relies on NIR observations from the Two Micron All-Sky Survey (2MASS) and new data from ESO's Vista Variables in the Via Lactea (VVV) survey, in concert with MIR observations from the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE). [2] The infrared archival data come from Galactic Legacy Infrared Midplane Survey Extraordinaire (GLIMPSE), Wide-field Infrared Survey Explorer (WISE) and Herschel InfraRed Galactic Plane Survey (HiGAL). [3]红外档案数据来自银河传统红外中平面巡天 (GLIMPSE)、银河多波段成像光度计巡天 (MIPSGAL) 和赫歇尔红外银河平面巡天 (Hi-GAL)。 [1] 新的灭绝地图的最大 bin 大小为 1'，并依赖于来自两微米全天巡天 (2MASS) 的 NIR 观测和来自 ESO 在 Via Lactea (VVV) 调查中的 Vista 变量的新数据，与 MIR 观测一致来自银河系遗产红外中平面非凡巡天 (GLIMPSE)。 [2] 红外档案数据来自银河传统红外中平面巡天 (GLIMPSE)、广域红外巡天探测器 (WISE) 和赫歇尔红外银河平面巡天 (HiGAL)。 [3]