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The limiting magnitudes with a slgnal-to-noise ratio of three in\u003cbr /\u003ethe deepest regions are 21.85 and 20.15 in the J- and Ks-bands respectively\u003cbr /\u003ein the Vega magnitude system.\u003cbr /\u003e\u003cbr /\u003e The J-and Ks-band galaxy counts in the AKARINEP field are broadly in\u003cbr /\u003egood agreement with those of other results in the literature, however the\u003cbr /\u003ecounts show a characteristic change in the galaxy count slope in both the J-and\u003cbr /\u003eKs-bands. The slope of the J-band galaxy counts per square degree per\u003cbr /\u003emagnitude clearly changes at J ~ 19.5 from d(logN)/dm = 0.39 ± 0.02 to\u003cbr /\u003e0.30 ± 0.03, while the ks-band galaxy counts shows a clear \u0027bump\u0027 in\u003cbr /\u003ethe magnitude range 18.0 \u003c Ks \u003c 19.5. The B -Ks color distribution of the\u003cbr /\u003egalaxy samples also shows an obvious change around the `bump\u0027\u003cbr /\u003emagnitude of the ks-band counts. The number of faint blue samples in the\u003cbr /\u003emagnitude range 18.5 \u003cKs \u003c 19.5 is signincantly larger than that of ks\u003c\u003cbr /\u003e17.5 samples.\u003cbr /\u003e\u003cbr /\u003e In order to find a clue tounderstandthe ongln of the change in J- and\u003cbr /\u003eks-band count slopes and the bluer trend at fainter magnitudes below the\u003cbr /\u003ebump of Ks-band counts, I also investigated the number counts of Ks-band\u003cbr /\u003eselected high redshift galaxy populations:the extremely red objects (EROs),\u003cbr /\u003ethe B,z and K-band selected galaxies (BzKs) and the distant red galaxies\u003cbr /\u003e(DRGs). I foundthat the number counts of both the passive EROs and the\u003cbr /\u003epassive BzKs have shallower slopes at fainter magnitudes and turnovers at\u003cbr /\u003eKs ~ 18.5 and Ks ~ 19.0, respectively, while the number count of the\u003cbr /\u003estar-fomlng BzKs is a single power-law with a steeper slope. The observed\u003cbr /\u003enumber counts of these passive populations are compared with a backward\u003cbr /\u003eevolution model allowing the number density evolution. The pure\u003cbr /\u003eluminosity evolution model without density evolution fails to explain the\u003cbr /\u003eobserved counts at faint magnitudes (Ks \u003e 17.0), while the model with a\u003cbr /\u003enegative density evolution is consistent with the observed counts of the\u003cbr /\u003epassive populations.\u003cbr /\u003e\u003cbr /\u003e Based on these results, I also investigated an evolutional scenario of\u003cbr /\u003egalaxy populations which can explainthe observed K-band count by using\u003cbr /\u003ethree components (early-type, late-type and star-forming populations),\u003cbr /\u003ebackward evolution model with type-dependent luminosity functions. I\u003cbr /\u003efound that not onlythe ellipticals but also the spiral galaxy population has\u003cbr /\u003eto follow the negative density evolution whilethe starburst population\u003cbr /\u003eshows the strong positive density evolution.\u003cbr /\u003e\u003cbr /\u003e Finally,the on-going NEP deep surveys at 2-26 pm with AKARI will\u003cbr /\u003eprovide us with new and critical pieces of information to verify and improve\u003cbr /\u003ethe galaxy evolution scenario discussed in this thesis.", "subitem_description_type": "Other"}]}, "item_1_description_7": {"attribute_name": "学位記番号", "attribute_value_mlt": [{"subitem_description": "総研大甲第986号", "subitem_description_type": "Other"}]}, "item_1_select_14": {"attribute_name": "所蔵", "attribute_value_mlt": [{"subitem_select_item": "有"}]}, "item_1_select_8": {"attribute_name": "研究科", "attribute_value_mlt": [{"subitem_select_item": "物理科学研究科"}]}, "item_1_select_9": {"attribute_name": "専攻", "attribute_value_mlt": [{"subitem_select_item": "11 宇宙科学専攻"}]}, "item_1_text_10": {"attribute_name": "学位授与年度", "attribute_value_mlt": [{"subitem_text_value": "2006"}]}, "item_creator": {"attribute_name": "著者", "attribute_type": "creator", "attribute_value_mlt": [{"creatorNames": [{"creatorName": "IMAI, Koji", "creatorNameLang": "en"}], "nameIdentifiers": [{"nameIdentifier": "0", "nameIdentifierScheme": "WEKO"}]}]}, "item_files": {"attribute_name": "ファイル情報", "attribute_type": "file", "attribute_value_mlt": [{"accessrole": "open_date", "date": [{"dateType": "Available", "dateValue": "2016-02-17"}], "displaytype": "simple", "download_preview_message": "", "file_order": 0, "filename": "甲986_要旨.pdf", "filesize": [{"value": "361.4 kB"}], "format": "application/pdf", "future_date_message": "", "is_thumbnail": false, "licensetype": "license_11", "mimetype": "application/pdf", "size": 361400.0, "url": {"label": "要旨・審査要旨", "url": "https://ir.soken.ac.jp/record/550/files/甲986_要旨.pdf"}, "version_id": "892b91e7-74a8-410f-82ec-2ea81a568e4e"}]}, "item_language": {"attribute_name": "言語", "attribute_value_mlt": [{"subitem_language": "eng"}]}, "item_resource_type": {"attribute_name": "資源タイプ", "attribute_value_mlt": [{"resourcetype": "thesis", "resourceuri": "http://purl.org/coar/resource_type/c_46ec"}]}, "item_title": "A NEAR INFRARED SURVEY IN THE AKARI NORTH ECLIPTIC POLE FIELD", "item_titles": {"attribute_name": "タイトル", "attribute_value_mlt": [{"subitem_title": "A NEAR INFRARED SURVEY IN THE AKARI NORTH ECLIPTIC POLE FIELD"}, {"subitem_title": "A NEAR INFRARED SURVEY IN THE AKARI NORTH ECLIPTIC POLE FIELD", "subitem_title_language": "en"}]}, "item_type_id": "1", "owner": "1", "path": ["13"], "permalink_uri": "https://ir.soken.ac.jp/records/550", "pubdate": {"attribute_name": "公開日", "attribute_value": "2010-02-22"}, "publish_date": "2010-02-22", "publish_status": "0", "recid": "550", "relation": {}, "relation_version_is_last": true, "title": ["A NEAR INFRARED SURVEY IN THE AKARI NORTH ECLIPTIC POLE FIELD"], "weko_shared_id": -1}
A NEAR INFRARED SURVEY IN THE AKARI NORTH ECLIPTIC POLE FIELD
https://ir.soken.ac.jp/records/550
https://ir.soken.ac.jp/records/550b70aece4-d4b7-4946-9a9c-2e4f94ddbd6c
名前 / ファイル | ライセンス | アクション |
---|---|---|
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Item type | 学位論文 / Thesis or Dissertation(1) | |||||
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公開日 | 2010-02-22 | |||||
タイトル | ||||||
タイトル | A NEAR INFRARED SURVEY IN THE AKARI NORTH ECLIPTIC POLE FIELD | |||||
タイトル | ||||||
言語 | en | |||||
タイトル | A NEAR INFRARED SURVEY IN THE AKARI NORTH ECLIPTIC POLE FIELD | |||||
言語 | ||||||
言語 | eng | |||||
資源タイプ | ||||||
資源タイプ識別子 | http://purl.org/coar/resource_type/c_46ec | |||||
資源タイプ | thesis | |||||
著者名 |
今井, 弘二
× 今井, 弘二 |
|||||
フリガナ |
イマイ, コウジ
× イマイ, コウジ |
|||||
著者 |
IMAI, Koji
× IMAI, Koji |
|||||
学位授与機関 | ||||||
学位授与機関名 | 総合研究大学院大学 | |||||
学位名 | ||||||
学位名 | 博士(理学) | |||||
学位記番号 | ||||||
内容記述タイプ | Other | |||||
内容記述 | 総研大甲第986号 | |||||
研究科 | ||||||
値 | 物理科学研究科 | |||||
専攻 | ||||||
値 | 11 宇宙科学専攻 | |||||
学位授与年月日 | ||||||
学位授与年月日 | 2006-09-29 | |||||
学位授与年度 | ||||||
2006 | ||||||
要旨 | ||||||
内容記述タイプ | Other | |||||
内容記述 | I present J- and Ks-band galaxy counts and galaxy colors covering 750<br />arcminutes<sup>2</sup> in the deep AKARI North Ecliptic Pole (NEP) field, using the<br />FLeridA Multi-object lmaglng Near-ir Grism Observational Spectrometer<br />(FLAMINGOS) on the Kitt Peak National Observatory (KPNO) 2.1 m<br />telescope. The limiting magnitudes with a slgnal-to-noise ratio of three in<br />the deepest regions are 21.85 and 20.15 in the J- and Ks-bands respectively<br />in the Vega magnitude system.<br /><br /> The J-and Ks-band galaxy counts in the AKARINEP field are broadly in<br />good agreement with those of other results in the literature, however the<br />counts show a characteristic change in the galaxy count slope in both the J-and<br />Ks-bands. The slope of the J-band galaxy counts per square degree per<br />magnitude clearly changes at J ~ 19.5 from d(logN)/dm = 0.39 ± 0.02 to<br />0.30 ± 0.03, while the ks-band galaxy counts shows a clear 'bump' in<br />the magnitude range 18.0 < Ks < 19.5. The B -Ks color distribution of the<br />galaxy samples also shows an obvious change around the `bump'<br />magnitude of the ks-band counts. The number of faint blue samples in the<br />magnitude range 18.5 <Ks < 19.5 is signincantly larger than that of ks<<br />17.5 samples.<br /><br /> In order to find a clue tounderstandthe ongln of the change in J- and<br />ks-band count slopes and the bluer trend at fainter magnitudes below the<br />bump of Ks-band counts, I also investigated the number counts of Ks-band<br />selected high redshift galaxy populations:the extremely red objects (EROs),<br />the B,z and K-band selected galaxies (BzKs) and the distant red galaxies<br />(DRGs). I foundthat the number counts of both the passive EROs and the<br />passive BzKs have shallower slopes at fainter magnitudes and turnovers at<br />Ks ~ 18.5 and Ks ~ 19.0, respectively, while the number count of the<br />star-fomlng BzKs is a single power-law with a steeper slope. The observed<br />number counts of these passive populations are compared with a backward<br />evolution model allowing the number density evolution. The pure<br />luminosity evolution model without density evolution fails to explain the<br />observed counts at faint magnitudes (Ks > 17.0), while the model with a<br />negative density evolution is consistent with the observed counts of the<br />passive populations.<br /><br /> Based on these results, I also investigated an evolutional scenario of<br />galaxy populations which can explainthe observed K-band count by using<br />three components (early-type, late-type and star-forming populations),<br />backward evolution model with type-dependent luminosity functions. I<br />found that not onlythe ellipticals but also the spiral galaxy population has<br />to follow the negative density evolution whilethe starburst population<br />shows the strong positive density evolution.<br /><br /> Finally,the on-going NEP deep surveys at 2-26 pm with AKARI will<br />provide us with new and critical pieces of information to verify and improve<br />the galaxy evolution scenario discussed in this thesis. | |||||
所蔵 | ||||||
値 | 有 |