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1.
利用碳星星表（ＧＣＧＣＳ）、红外天文卫星（ＩＲＡＳ）点源表（ＰＳＣ）、哈勃望远镜（ＨＳＴ）导星星表（ＧＳＣ）及美国海军天文台星表（ＵＳＮＯ）对现今已知的２２个硅酸盐碳星重新进行了交叉证认,给出它们的确切位置,以利于今后进一步的观测研究,同时也指出其中存在值得怀疑的对象 相似文献
2.
本文使用ＩＲＡＳ巡天数据的最新版本ＩＲＡＳ巡天图（ＩＳＳＡ），经过进一步处理，得到了Ｓ１４１分子云复合体红外发射的强度、温度及尘埃的分布图。分析结果表明，分子云复合体（在１５角秒的统计范围内）的红外发射总光度为１．７１×１０３Ｌ⊙，热而小的尘埃微粒的平均色温是１７８．５Ｋ，冷而大的尘埃平均色温为２６．８Ｋ。分子云复合体中有三个明显的密集发射区，在东北边缘另有一相对弱的密度发射区。分析表明，Ｓ１４０电离氢区—分子云复合体中很可能有低质量呈正在形成。电离氢区Ｓ１４１的激发星很可能是位于其边缘的红外点源２２２６８＋６１２２的光学对应体。 相似文献
3.
利用Ｒ（红）－Ⅰ（近红外）两色照相测光方法，搜寻银道整天区的红外超天体，并证认ＩＲＡＳ点源的红外超对应体。本是一组系列章的第四篇。在矩尺天区发现了１９５个红外超天体，并证认出其中２２个是ＩＲＡＳ点源的对应体。 相似文献
4.
利用Ｒ（红）－Ｉ（近红外）两色照相测光方法，搜寻银道带天区的红外超天体，并证认ＩＲＡＳ点源的红外超对应体。本文是一组系列文章的第四篇。在矩尺天区发现了１９５个红外超天体，并证认出其中２２个是ＩＲＡＳ点源的对应体。 相似文献
5.
利用北京天文台具有ＣＣＤ终端的６０ｃｍ光学望远镜观测射电源的光学对应体，得到了０１７１６＋７１４和０８３９＋１８７精确的光位置。参考星表采用拉帕玛的１８ｃｍ全自动子午环观测资料编制的ＣＡＭＣ星表，该星表是ＦＫ５星表系统。 相似文献
6.
利用北京天文台具有ＣＣＤ终端的６０ｃｍ光学望远镜（Ｖ波段）观测射电源的光学对应体，得到了０７１６＋７１４和０８３９＋１８７精确的光学位置。参考星表采用拉帕尔玛（ＬａＰａｌｍａ）的１８ｃｍ全自动子午环观测资料编制的ＣＡＭＣ星表，该星表是ＦＫ５星表系统。两颗源位置的内符精度约为０．″１９，与其他作者给出的光学和射电位置观测结果分别进行了比较 相似文献
7.
本论文用ＩＲＡＳ巡天数据的最新版本ＩＳＳＡ，经过进一步处理，得到了Ｓ１４０、Ｓ１４１、Ｓ１４２ＳｈａｒｐｌｅｓｓＨⅡ区—分子云复合体的红外发射强度、温度及其光深的分布图。在此基础上对各ＨⅡ区的特性参量进行了统计分析，得到了分子云复合体的红外发射总光度以及复合体中尘埃的分布情况，对尘埃中ＶＳＧ的丰度作出了分析。并对各恒星形成区中的致密团块进行了研究，揭示出其中一些可能的恒星形成区域。同时对Ｓ１４０区中的有关红外点源作出了能谱分折，并对Ｓ１４１区的激发星进行了讨论。第一章对红外天文学研究及其特点作出了分析，并集中介绍了ＨⅡ区的有关情况；第二章给出了ＩＲＡＳ红外天文卫星及其数据资料的一些情况；第三章、第四章和第五章，重点给出了ＩＳＳＡ图像资料的处理和各ＨⅡ区的征对性分析及所得结论。文中图像分析所用的一些辅助工具（如用于ＩＳＳＡ定位分析的ＩＲＡＦ坐标系和赤道坐标系的转换程序等）出于作者之手，另外，本文分析所用红外天空巡天图由ＩＰＡＣ提供，而红外发射强度图、红外色温和光深分布图以及有关统计分析则隶属于作者的图像处理结果。 相似文献
8.
利用瑞士Ｇｏｒｎｅｒｇｒａｔ天文台的意大利１．５米ＴＩＲＧＯ红外望远镜对近红外交源ＩＲＡＳ０４０００＋５０５２进行了近红外成像观测,得到了ＪＨＫ宽带及Ｈ２Ｓ（１）１～０和Ｂｒ窄带高分辨率图像,并进行了红外测光及位置测量工作．结果发现此ＩＲＡＳ源不是以往认为的单一年轻天体,而是一个包含有许多个年轻天体的小尺度致密恒星形成区,在这样小尺度且致密区域内,恒星形成也不是在同一时期完成的． 相似文献
9.
利用瑞士Ｇｏｒｎｅｒｇｒａｔ天文台的意大利１．５米ＴＩＲＧＯ红外望远镜对近红外变源ＩＲＡＳ０４０００＋５０５２进行了近红外成像观测,得到了ＪＨＫ宽带及Ｈ２Ｓ（１）１￣０和Ｂｒγ窄带高分辨率图像,并进行了红外测光及位置测量工作。结果发现此ＩＲＡＳ源不是以往认为的单一年轻天体,而是一个包含有许多个年轻天体的小尺度致密恒星形成区,在这样小尺度且致密区域内,恒星形成也不是在同一时期完成的。 相似文献
10.
给出２６ 个金牛Ｔ 型星的ＩＲＡＳ低分辨率红外光谱．根据这些光谱讨论了它们有关的性质和所处环境．分析发现硅酸盐尘埃在金牛Ｔ 型星拱星壳层中是常见的物质 相似文献
11.
Kyung-Won Suh 《Monthly notices of the Royal Astronomical Society》2000,315(4):740-750
We have investigated the optical properties of the carbon dust grains in the envelopes around carbon-rich asymptotic giant branch stars, paying close attention to the infrared observations of the stars and the laboratory-measured optical data of the candidate dust grain materials. We have compared the radiative transfer model results with the observed spectral energy distributions of the stars including IRAS Point Source Catalog and IRAS Low Resolution Spectrograph data. We have deduced an opacity function of amorphous carbon dust grains from model fitting with infrared carbon stars. From the opacity function, we have derived the optical constants of the AMC grains. The optical constants satisfy the Kramers–Kronig relation and produce the opacity function that fits the observations of infrared carbon stars better than previous works in the wide wavelength range 1–1000 μm. We have used simple mixtures of the AMC and silicon carbide grains for modelling. We have compared the contributions that AMC and SiC grains make to the opacity for the cases of simple mixtures of them and spherical core–mantle type grains consisting of a SiC core and an AMC mantle . 相似文献
12.
A fourth list of point sources from the IRAS Point Source Catalog (PSC) that are optically identified with stars of late spectral
types is given. The list contains data on 41 objects. The identifications were based on the Digital Sky Survey (DSS), the
First Byurakan Survey, blue and red maps of the Palomar Observatory Sky Survey, and infrared fluxes at the wavelengths 12,
25, 60, and 100 μm in the region of +65° ≤ δ ≤ +69° and 05h10m ≤ α ≤ 18h10m. Of the 41 objects, which are given in the IRAS PSC as unidentified sources of infrared emission, 9 are associated with known
stars in existing catalogs while 32 sources remained unidentified in the optical range, one of which is also a source in the
deep IRAS survey (IRAS Serendipitous Source Catalog). The optical coordinates, their departures from the IR coordinates, the
V stellar magnitudes, the color indices CI, and the preliminary spectral subtypes have been determined. The objects have optical
magnitudes in the range of 8m.5-14m.5. Finder charts from the DSS are given for 32 of the objects.
Translated from Astrofizika, Vol. 43, No. 3, pp. 361-368, July–September, 2000. 相似文献
13.
A third list of point sources from the IRAS Point Source Catalog (PSC), optically identified with late-type stars, is given.
The list contains data on 34 objects. The identification was based on the Digitized Sky Survey (DSS), the First Byurakan Survey
(FBS). blue and red maps of the Palomar Observatory Sky Survey, and infrared fluxes at wavelengths of 12, 25, 60, and 100
mm in the regions of +61° ≤ δ ≤ +65°, 06h45m ≤ α ≤ 17h28m and +69° ≤ δ ≤ +73°, 03h50m ≤ α ≤ 18h10m. Of 34 objects given in the IRAS PSC as unidentified sources of infrared radiation, 11 are associated with known stars in
existing catalogs, 6 are objects from the FBS survey of late-type stars, and 17 sources remained unknown in the optical range,
3 of them also being sources in the IRAS Serendipitous Survey Catalog (SSC). The optical coordinates, their departures from
the 1R coordinates, the V magnitudes, the color indices CI, and the preliminary spectral subtypes were determined. The objects
have optical magnitudes in the range of 7h.6-13m.6. Finder charts from the DSS are given for 23 objects.
Translated from Astrofizika, Vol. 43, No. 1, pp. 77-84, January–March, 2000. 相似文献
14.
O. Hashimoto H. Izumiura D. J. M. Kester Tj. R. Bontekoe 《Astrophysics and Space Science》1995,224(1-2):477-478
Extended emission components are clearly found in the IRAS scan data of optically visible oxygen-rich AGB stars which show no 10µm silicate band feature in the IRAS LRS spectra but a strong infrared excess in the IRAS photometric data. It is most likely that these stars really have their circumstellar dust envelopes, which are detached from the central stars, indicating a halting of mass loss for a significant period. 相似文献
15.
Chen Pei-sheng Gao Heng Bao Meng-xian Xiong Guang-zhu 《Chinese Astronomy and Astrophysics》1992,16(4):399-406
The JHKL' photometry and 2.3–4 μm spectrophotometry of some M giants, S type stars and carbon stars are presented in this paper. It is found that in combination with IRAS data, the energy spectra in 1–100 μm of S type stars are intermediate between those of M giants and carbon stars, which are obviously different. The spectrophotometry in the near infrared shows that, besides carbon stars, which have HCN and C2H2 strong absorptions at 3.1 μm, some S type stars have the similar but weaker absorption in the same spectral region. However, no trace of any absorption at 3.1 μm can be seen in M giants. These results probably provide more evidence for the M-S-C sequence in the late stage of stellar evolution. 相似文献
16.
We collected 55 galactic extreme carbon stars from the published literature in this paper. Observational data from IRAS, 2MASS
and ISO were analyzed. The results show that the infrared properties of extreme carbon stars are quite different to those
for ordinary visual carbon stars. It is shown from IRAS and 2MASS photometric data that extreme carbon stars have much redder
infrared colors not only in the far infrared, but also in the near infrared, hence they have much thicker ciucumstellar envelopes
and mass loss. It is also indicated from IRAS Low-Resolution Spectra (LRS) and ISO Short Wavelength Spectra (SWS) that they
have much redder infrared spectra from 2 μm to 45 μm. The above results are believed to be the signature of undergoing the
last stages of AGB evolution for extreme carbon stars. 相似文献
17.
A 10th list of late-type M and C stars found on plates of the First Byurakan Spectral Sky Survey in the − 11° ≤ δ ≤ − 7° belt
with an area of about 1070 deg2 is given. The list contains data on 169 red stars, 117 of which were found for the first time: 8 are new C stars, 3 are Cstar
candidates, 104 are M stars, 1 is either an M or an S star, and 1 object on the survey plate cannot be classified. Of the
117 objects, 47 are unidentified IRAS sources. A statistical analysis of the objects that are and are not identified with
IRAS sources shows that the identified stars are, with a high probability, brighter and have relatively more massive envelopes.
Two stars were found to have fairly large brightness variability (with an amplitude of at least 6m.O). Gasdust shells are assumed to exist around nine of the IRAS sources. The equatorial coordinates, spectral types, and
stellar magnitudes, determined on Palomar E maps, are given for the selected objects.
Translated from Astrofizika, Vol. 41. No. 4, pp. 545–559, October–December, 1998. 相似文献
18.
《New Astronomy》2021
We have collected almost all HdC, RCB and EHe stars up to date to investigate their infrared properties, in particular, their radiation mechanisms in the infrared, using the observational data from 2MASS, WISE and IRAS missions. Because HdC stars, RCB stars and EHe stars all belong to the category of extremely hydrogen-deficient stars and they definitely have some evolutionary connections.It is found from this paper that all RCB stars have infrared excesse in the wavelength region from the near infrared to the far infrared covered by 2MASS, WISE and IRAS due to dust while almost all HdC stars and EHe stars have no or little infrared excess.From 2MASS, WISE and IRAS two-color diagrams, it is also found that the majority of these three kinds of stars are around the power law distributions in the near infrared possibly indicative of their infrared radiations from the warm dust in the disk-like envelope. It is also found that in the mid- and far infrared regions some stars are around the power law distribution perhaps due to dust from disk-like envelope while some stars are around the blackbody distribution maybe due to the cold and extended nebulosity nearby. 相似文献
19.
The IRAS and 2MASS associations for 206 HAEBE stars are identified in this paper. From the color-color diagrams and spectral index, it is found that the IR excesses for most samples are due to thermal emission from the circumstellar material. It is also found that the IR excesses at IRAS region for few HAEBE stars and the near-IR excesses for some HAEBE stars are likely attributed to free-free emission or free-bound emission from the circumstellar ionized gas. Moreover, the evolution scenario (from embedded HAEBE stars to β Pictoris-like main-sequence stars) from Malfait et al. (1998) has been checked, our result does not support this evolution scenario.This publication makes use of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, founded by the National Aeronautics and Space Administration and the National Science Foundation of the United States. 相似文献
20.
The power spectrum estimator based on the Discrete Wavelet Transformation (DWT) is applied to detect the clustering power in the IRAS Point Source Catalog Redshift Survey(PSCz). Comparison with mock samples extracted from N-body simulation shows that the DWT power spectrum estimator could provide a robust measurement of banded fluctuation power over a range of wavenumbers 0.1-2.0h Mpc^-1. We have fitted three typical CDM models (SCDM, TCDM and ACDM) using the Peacock-Dodds formula including non-linear evolution and redshift distortion. We find that, our results are in good agreement with other statistical measurements of the PSCz. 相似文献