This paper provides a detailed description of the data reduction and analysis procedures that have been employed in our previous studies of spatial fluctuation of the cosmic infrared background (CIB) using deep Spitzer IRAC observations. The self-calibration we apply removes a strong instrumental signal from the fluctuations which would otherwise corrupt our results. The procedures and results for masking bright sources, and modeling faint sources down to levels set by the instrumental noise are presented. Various tests are performed to demonstrate that the resulting power spectra of these fields are not dominated by instrumental or procedural effects. These tests indicate that the large scale (>~30') fluctuations that remain in the deepest fields are not directly related to the galaxies that are bright enough to be individually detected. We provide the parameterization of these power spectra in terms of separate instrument noise, shot noise, and power law components. Our measurements of spatial fluctuations of the CIB intensity indicate the mean emission from the objects producing the fluctuations is quite low (>~1 nW m-2 sr-1 at 3-5 micron), and thus consistent with current gamma-ray absorption constraints. The source of the fluctuations may be high-z Population III objects, or a more local component of very low luminosity objects with clustering properties that differ from the resolved galaxies. Finally, we discuss the prospects of the upcoming space-based surveys to directly measure the epochs inhabited by the populations producing these source-subtracted CIB fluctuations, and to isolate the individual fluxes of these populations.
This paper describes new deep 3.6 and 4.5 micron imaging of three UltraVISTA near-infrared survey stripes within the COSMOS field. The observations were carried out with Spitzer's Infrared Array Camera (IRAC) for the Spitzer Matching Survey of the Ultra-VISTA Deep Stripes (SMUVS). In this work we present our data reduction techniques, and document the resulting mosaics, coverage maps, and catalogs in both IRAC passbands for the three easternmost UltraVISTA survey stripes, covering a combined area of about 0.66 square degrees, of which 0.45 square degrees have at least 20 hr integration time. S…
S-CANDELS: The Spitzer-Cosmic Assembly Near-Infrared Deep Extragalactic Survey. Survey Design, Photometry, and Deep IRAC Source Counts
斯皮策宇宙大会深近红外河外遗产调查（S-CANDELS; PI G。Fazio）是一个第8周期的探索计划，旨在探测非常高红移（z > 5）的星系。为了减轻宇宙变化的影响，并利用哈勃空间望远镜多周期财政计划CANDELS在多个波段的深度同延覆盖，S-CANDELS在五个相距甚远的河外区域进行：UKIDSS超深巡天、扩展钱德拉深场南、COSMOS、HST深场北和扩展格罗斯带。S-CANDELS建立在斯皮策扩展深度调查（SEDS）现有的这些领域的覆盖范围之上，将积分时间从12小时增加到总共50小时，但在较小的区域内，0.16平方度。额外的深度显著增加了微弱星等下的勘测完整性。本文介绍了S-CANDELS调查的设计、处理和公开提供的数据产品。我们目前的IRAC双波段3.6+4.5微米目录达到26.5 AB MAG的深度。深IRAC计数的大约135,000个星系检测的S-CANDELS是一致的模型的基础上已知的星系种群。比早期斯皮策/IRAC调查更深的深度增加并没有揭示离散源对弥漫的宇宙红外背景（CIB）的显着额外贡献。因此，它仍然是正确的，只有大约一半的估计CIB通量从COBE/DIRBE解决。
We study the stellar population properties of the IRAC-detected $6 \lesssim z \lesssim 10$ galaxy candidates from the Spitzer UltRa Faint SUrvey Program (SURFS UP). Using the Lyman Break selection technique, we find a total of 16 new galaxy candidates at $6 \lesssim z \lesssim 10$ with $S/N \geq 3$ in at least one of the IRAC $3.6μ$m and $4.5μ$m bands. According to the best mass models available for the surveyed galaxy clusters, these IRAC-detected galaxy candidates are magnified by factors of $\sim 1.2$--$5.5$. We find that the IRAC-detected $6 \lesssim z \lesssim 10$ sample is likely not a h…
We present the first detailed analysis of three extragalactic fields (IRAC Dark Field, ELAIS-N1, ADF-S) observed by the infrared satellite, AKARI, using an optimised data analysis toolkit specifically for the processing of extragalactic point sources. The InfraRed Camera (IRC) on AKARI complements the Spitzer space telescope via its comprehensive coverage between 8-24 microns filling the gap between the Spitzer IRAC and MIPS instruments. Source counts in the AKARI bands at 3.2, 4.1, 7, 11, 15 and 18 microns are presented. At near-infrared wavelengths, our source counts are consistent with coun…
Spitzer IRAC Low Surface Brightness Observations of the Virgo Cluster
我们目前的3.6和4.5微米斯皮策IRAC成像超过0.77平方度的室女星系团核心的目的是了解低表面亮度的形成机制的集群内的光功能。比信号高出数百倍的仪器和天体物理背景被仔细表征和去除。我们研究了巨大椭圆星系M87的团内光羽和外晕。对于两个团内光羽，我们使用光学颜色来限制它们的年龄分别大于3和5 Gyr。IRAC通量的上限限制了质量的上限，光学检测限制了质量的下限。在这第一次测量团内轻羽流的质量时，我们发现我们所覆盖的两个羽流的质量范围分别为5.5 x 10^8 - 4.5 x 10^9和2.1 x 10^8 - 1.5 x 10^9太阳质量。考虑到它们的预期寿命很短，以及这些类型的流的恒定生产率，在室女座的一生中，它们可以解释星团的ICL总含量，这意味着我们不需要调用ICL形成机制，而不是引力机制导致明亮的羽流。我们还研究了巨大的椭圆形M87的外晕。从M87的内晕到外晕（160 Kpc）的颜色轮廓与平坦或光学蓝色梯度一致，其中蓝色梯度可能是由于更年轻或更低的金属量恒星在更大的半径。由红外和光学颜色预测的年龄的相似性（>几Gyr）表明，光学测量并没有强烈的尘埃消光的影响。
We describe the first data release from the Spitzer-IRAC Equatorial Survey (SpIES); a large-area survey of 115 deg^2 in the Equatorial SDSS Stripe 82 field using Spitzer during its 'warm' mission phase. SpIES was designed to probe sufficient volume to perform measurements of quasar clustering and the luminosity function at z > 3 to test various models for "feedback" from active galactic nuclei (AGN). Additionally, the wide range of available multi-wavelength, multi-epoch ancillary data enables SpIES to identify both high-redshift (z > 5) quasars as well as obscured quasars missed by optical su…
Using the first epoch of four-band NIRCam observations obtained by the James Webb Space Telescope (JWST) Prime Extragalactic Areas for Reionization and Lensing Science Program in the Spitzer IRAC Dark Field, we search for F150W and F200W dropouts. In 14.2 arcmin^2, we have found eight F150W dropouts and eight F200W dropouts, all brighter than 27.5 mag (the brightest being ~24 mag) in the band to the red side of the break. As they are detected in multiple bands, these must be real objects. Their nature, however, is unclear, and characterizing their properties is important for realizing the full…
The IRAC mapping of the NMBS-II fields program is an imaging survey at 3.6 and 4.5$μ$m with the Spitzer Infrared Array Camera (IRAC). The observations cover three Canada-France-Hawaii Telescope Legacy Survey Deep (CFHTLS-D) fields, including one also imaged by AEGIS, and two MUSYC fields. These are then combined with archival data from all previous programs into deep mosaics. The resulting imaging covers a combined area of about 3 $deg^2$, with at least $\sim$2 hr integration time for each field. In this work, we present our data reduction techniques and document the resulting coverage maps at…
