Erratum: “Molecular Gas in Infrared-Excess, Optically Selected Quasars and the Connection with Infrared-Luminous Galaxies” [Astron. J. 121, 1893 (2001)]
Erratum: “Molecular Gas in Infrared-Excess, Optically Selected Quasars and the Connection with Infrared-Luminous Galaxies” [Astron. J. 121, 1893 (2001)]
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勘误：“红外过量的分子气体、光学选择类星体以及与红外发光星系的联系”[Astron J. 121, 1893 (2001)]
DOI：
10.1086/321098
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发表时间：
2001
期刊：
影响因子：
--
通讯作者：
D. Sanders
中科院分区：
文献类型：
--
作者：
A. Evans;D. Frayer;J. Surace;D. Sanders
本文给出了Palomar-Green(PG)亮类星体探测中红移在0.04\z\0.17范围内的红外过量类星体的毫米波(CO)测量的初步结果。这些观测代表着第一步，用完整的样本来确定准恒星物体(QSO)是否存在于富分子气体星系中，以及确定类星体的红外和分子气体性质与超发光红外星系(ULIGs)的红外和分子气体性质的比较，后者可能是类星体的演化前身。样本由绝对蓝色星等和红外过度(即红外到“”大蓝凸II MB[[22.0光度)，Km)[0.36]组成，其中对测热流明IR(8E1000公里)/L BBB(0.1E1.0)的贡献通常为20%E40%。在观测到的十个类星体中，有六个是在CO(1]0)发射线上探测到的；两次探测与先前在PG 1613]658和0838]770中对CO(1]0)较不灵敏的探测相一致，另外四个类星体是首次探测到的(PG 1119]120,1351]640,1415]451和1440]356)。这6次探测，加上之前在I Zw 1和MRK 1 0 14中探测到的2次CO，使迄今在CO中探测到的0.0 4-0.17个红外对流PG类星体总数达到8个，并提供了可能的证据，表明分子气体除了促进恒星形成外，还可能是类星体活动的主要燃料来源。在CO中探测到的8个类星体和未探测到的4个类星体相对于大多数红外发光星系都具有较高的红外/CO光度比L IR/L CO@，L IR这些类星体在平面上的位置可能是由于其所在星系中由L IR/L CO@EL IR类星体加热的尘埃的显著贡献，这是由于相对于大多数红外发光星系而言，由高效率(即单位分子气体质量)形成的大质量恒星加热的尘埃，或两者的结合。如果观测到的高值主要是由于类星体对尘埃的加热，则有相当一部分L IR/L CO@ULIGs具有相似的值也可能含有被掩埋的活动星系核。或者，如果L IR/L CO@HIGH主要是由于恒星的形成，那么恒星形成率的提高可能与L IR/L CO@与类星体现象密切相关。8个探测到的和4个未探测到的类星体的红外和CO发光度与其所在星系的光学形态的比较表明，3个具有和类似于ULIGs的类星体似乎位于形态扰动的星系L IR L CO@(即涉及两个或更多富气盘状星系的正在进行的重大合并)中，而其余8个类星体的宿主星系处于较低的位置，似乎是由条状螺旋宿主星系、L IR L CO@椭圆星系、分类不确定的星系和至少一次正在进行的重大合并组成的混合体。
The initial results of a millimeter (CO) survey of infrared-excess, optically selected quasars from the Palomar-Green (PG) Bright Quasar Survey with redshifts in the range 0.04\ z\ 0.17 are presented. These observations represent the Ðrst step toward establishing with a complete sample whether or not quasi-stellar objects (QSOs) reside in molecular gasErich galaxies, as well as determining how the infrared and molecular gas properties of QSOs compare with those of ultraluminous infrared galaxies (ULIGs), which are a possible evolutionary precursor of QSOs. The sample consists of QSOs having absolute blue magnitudes and infrared excesses (i.e., infrared to ““ big blue bump II M B [[22.0 luminosity), km)[ 0.36, in which the contribution to the bolometric lumiL IR(8E1000 km)/L bbb(0.1E1.0 nosity of infrared thermal dust emission for all PG QSOs is typically 20%E40%. Six out of ten of the QSOs observed are detected in the CO (1] 0) emission line ; two detections conÐrm previous, less sensitive detections of CO (1] 0) in PG 1613]658 and 0838]770, and four additional QSOs are detected for the Ðrst time (PG 1119]120, 1351]640, 1415]451, and 1440]356). These six detections, plus two previous detections of CO in I Zw 1 and Mrk 1014, bring the total number of 0.04\ z\ 0.17 infraredexcess PG QSOs detected in CO to date to eight and provide possible evidence that, in addition to fueling star formation, molecular gas may also serve as a primary source of fuel for QSO activity. Both the eight QSOs detected in CO and the four QSOs with nondetections have high infrared-to-CO luminosity ratios, relative to most infrared-luminous galaxies of the same The placement of L IR/L CO @ , L IR these QSOs on the plane may be due to signiÐcant contributions from dust heated by the L IR/L CO @ EL IR QSO in their host galaxies, due to dust heated by massive stars formed with high efficiency (i.e., per unit molecular gas mass) relative to most infrared-luminous galaxies, or a combination of both. If the observed high values of are primarily due to dust heating by QSOs, a signiÐcant fraction of L IR/L CO @ ULIGs with similar values of may also contain buried active galactic nuclei. Alternatively, if L IR/L CO @ high is due primarily to star formation, then an enhanced star formation rate may be intimately L IR/L CO @ connected to the QSO phenomenon. A comparison of the infrared and CO luminosities of the eight detected and four undetected QSOs with the optical morphologies of their host galaxies shows that the three QSOs with and similar to ULIGs appear to reside in morphologically disturbed galaxies L IR L CO @ (i.e., ongoing major mergers involving two or more gas-rich disk galaxies), whereas the host galaxies of the remaining eight QSOs with lower and appear to be a mixture of barred spiral host galaxies, L IR L CO @ elliptical galaxies, galaxies with an indeterminate classiÐcation, and at least one ongoing major merger.