射电类星体的演化与宇宙学红移*

熊定荣，张 雄，郑永刚，刘文广，康 婷，郭 飞

(云南师范大学物理与电子信息学院，云南 昆明 650092)

射电类星体演化的实质是指天体在宇宙时标上的变化，而天体的宇宙时标主要与宇宙学红移有关[1]。在天体演化的过程中，各个阶段的宇宙学红移不同，因此可以根据宇宙学红移确定天体的演化。 射电类星体按照射电辐射强度的不同可以分为射电噪类星体(Radio Loud Quasars, RLQ)和射电宁静类星体(Radio Quiet Quasars, RQQ)[2]，一般用射电噪度(Radio Loudness)等于10来区分射电宁静和射电噪类星体；射电噪度大于10称为射电噪类星体；小于10称为射电宁静类星体[3]。然而到底是指向效应还是内秉的演化结果造成了射电宁静和射电噪类星体本质的不同，目前还在研究中，这也是构造活动星系核统一结构和演化模型时遇到的最大问题之一。 Punsly(1996)和Park(1988)模型中提出了类星体到Seyfert星系的演化[4-5]，但这一演化一直没有得到很好的验证。核占优型射电类星体和瓣占优型射电类星体之间是否存在演化关系对射电喷流的研究也具有重要意义。基于这些研究背景，收集和计算了许多射电宁静类星体、射电噪类星体和Seyfert星系的重要参数，做出了这些参数和红移的关系图，利用Logistic非线性回归分析的方法对射电类星体的演化进行拟合，得出相应的演化曲线。

1 样本选取和数据处理

表1 射电类星体样品

续 表

NameTypeZlogLbollogMref mlogSref0159-117RLQ0.66946.849.2780.37150.143160210+860RLQ0.18644.926.5482.39880221+067RLQ0.5144.947.2980.4467-0.113170327-241RLQ0.88846.018.680.257-0.137170336-019RLQ0.85246.328.9880.21880.456160403-132RLQ0.57146.479.0780.25120.459160405-123RLQ0.57447.49.4780.85110.292160420-014RLQ0.915479.0380.93330.164160437+785RLQ0.45446.158.7980.22910444+634RLQ0.78146.128.5380.3890454+066RLQ0.40545.127.4280.5012-0.357170454-810RLQ0.44445.328.1380.15490502+049RLQ0.95446.368.8880.302-0.097170514-459RLQ0.19445.367.5580.64570518+165RLQ0.75946.348.5380.64570.614160538+498RLQ0.54546.439.5880.07080.919160602-319RLQ0.45245.699.0280.04680.0969160607-157RLQ0.32446.38.6880.41690.260160637-752RLQ0.65447.169.4180.56230.767160646+600RLQ0.45545.588.7480.06920723+679RLQ0.84646.418.6780.54950.121160736+017RLQ0.19145.97880.93330.299160738+313RLQ0.63146.949.480.34670.396160809+483RLQ0.87146.547.9683.80190.645160838+133RLQ0.68446.238.5280.51290.143160906+430RLQ0.66845.997.981.23030.255160912+029RLQ0.42745.267.7280.3467-0.337170923+392RLQ0.69846.269.2880.09550.941160925-203RLQ0.34846.358.4680.7762-0.155170953+254RLQ0.71246.59980.3890.260160954+556RLQ0.90146.548.0782.95120.358161004+130RLQ0.2446.219.180.12881007+417RLQ0.61246.718.7980.8318-0.149161016-311RLQ0.79446.638.8980.5495-0.187171020-103RLQ0.19744.878.3680.0324-0.310171034-293RLQ0.31246.28.7580.28180.179161036-154RLQ0.52544.557.880.0562-0.108171100+772RLQ0.31146.499.3180.1514-0.113161101-325RLQ0.35546.338.6180.5248-0.137171106+023RLQ0.15744.977.580.2951-0.301171107-187RLQ0.49744.256.980.2239-0.301171111+408RLQ0.73446.269.8280.0275-0.102161128-047RLQ0.26644.086.7280.2291-0.046171136-135RLQ0.55446.788.78810.324161137+660RLQ0.65646.859.3680.3090.025161150+497RLQ0.33445.988.7380.17780.04916

续 表

NameTypeZlogLbollogMref mlogSref1151-348RLQ0.25845.569.0280.03471200-051RLQ0.38146.418.4181-0.337171202-262RLQ0.78945.81980.0646-0.004171217+023RLQ0.2445.838.4180.2631226+023RLQ0.15847.357.2282.03191.632161237-101RLQ0.75146.639.2880.22390.117161244-255RLQ0.63346.489.0480.27541250+568RLQ0.32145.618.4280.15490.025161253-055RLQ0.53646.18.4380.46771.176161254-333RLQ0.1945.528.8380.049-0.268171302-102RLQ0.28645.868.380.36310.068161352-104RLQ0.33245.818.1580.4571-0.009171354+195RLQ0.7247.119.4480.46770.193161355-416RLQ0.31346.489.7380.05620.158161359-281RLQ0.80346.918.0786.9183-0.174171450-338RLQ0.36843.946.4680.302-0.268171451-375RLQ0.31446.168.8280.21881458+718RLQ0.90546.938.9880.89131509+022RLQ0.21944.547.9980.0355-0.268171510-089RLQ0.36146.388.6580.5370.489161545+210RLQ0.26645.868.9380.0851-0.14391546+027RLQ0.412468.7280.19050.161161611+343RLQ1.40146.999.5780.2630.427161634+628RLQ0.98845.477.2881.54881637+574RLQ0.7546.689.1880.31620.152161641+399RLQ0.59446.899.4280.29511.033161642+690RLQ0.75145.787.7681.04710.143161656+053RLQ0.87947.219.6280.3890.322171704+608RLQ0.37146.338.2381.25890.090161706+006RLQ0.44944.016.6380.2399-0.420171721+343RLQ0.20645.638.0480.389-0.032161725+044RLQ0.29346.078.07810.093161726+455RLQ0.71445.858.2280.42661828+487RLQ0.69146.789.8580.08510.792161849+670RLQ0.65746.239.1480.1231856+737RLQ0.4646.218.8980.20891928+738RLQ0.30246.688.9180.58880.524161954-388RLQ0.62646.318.6380.47860.314162004-447RLQ0.2445.327.4880.6918-0.187172043+749RLQ0.10446.239.6280.04072059+034RLQ1.01246.849.1380.5129-0.125172111+801RLQ0.52445.838.7380.12592120+099RLQ0.93245.758.1980.3631-0.301172128-123RLQ0.50146.769.6180.14130.316162135-147RLQ0.246.178.9480.16980.149162141+175RLQ0.21346.238.7480.309-0.46618

续 表

NameTypeZlogLbollogMref mlogSref2155-152RLQ0.67245.677.5981.20230.199172201+315RLQ0.29846.628.8780.56230.365162216-038RLQ0.90147.179.2480.85110.176162247+140RLQ0.23745.477.5980.75860.009162251+158RLQ0.85947.279.1781.25891.241162255-282RLQ0.92646.969.1680.6310.238172311+469RLQ0.74146.559.380.1778-0.137162329-415RLQ0.67146.228.9380.195-0.328172344+092RLQ0.67347.079.3180.57540.155162345-167RLQ0.57645.928.7280.15850.563162349-014RLQ0.17345.948.7880.14452355-082RLQ0.2145.018.3980.0417

表2 Seyfert星系样品

续 表

NameTypeZlogLbollog mNameTypeZlogLbollog mNGC7672SY0.01343.866.880.0955NGC3998SY0.00343.548.950.0004NGC7682SY0.01743.937.280.0447Mrk10SY0.02944.617.470.138NGC7743SY0.00643.66.590.1023UGC3223SY0.01644.277.020.1778Mrk1SY0.01644.27.160.1096NGC3227SY0.00443.867.640.0166Mrk3SY0.01444.548.650.0078NGC3516SY0.00944.297.360.0851Mrk78SY0.03744.597.870.0525NGC3783SY0.0144.416.940.2951Mrk270SY0.0143.377.60.0059NGC4051SY0.00243.566.130.2692Mrk348SY0.01544.277.210.1148NGC4151SY0.00343.737.130.0398Mrk533SY0.02945.157.560.389NGC4253SY0.01344.46.540.7244Mrk573SY0.01744.447.280.1445NGC4593SY0.00944.096.910.1514Mrk622SY0.02344.526.920.3981NGC5548SY0.01744.838.030.0631Mrk686SY0.01444.117.560.0355NGC6814SY0.00543.927.280.0437Mrk917SY0.02444.757.620.1349NGC7469SY0.01645.286.842.7542

表3 核占优和瓣占优型射电类星体样品

续 表

NameZ射电形态logRNameZ射电形态logR0007+3320.743LDQ-1.71623+1730.552LDQ-0.80044+0300.624LDQ0.211704+608*0.371LDQ-0.970118+0340.765LDQ-0.511741+2790.372LDQ-0.250127+2331.46LDQ-1.721807+2791.76LDQ0.150159-117*0.669LDQ1.041830+2850.594LDQ0.360238+1001.816LDQ-0.821857+5661.595LDQ-1.290300-0040.693LDQ0.981924+5071.098LDQ0.320307+4441.165LDQ-0.442005-0440.589LDQ-0.560340+0480.357LDQ-1.122209+0800.484LDQ-0.370349-1460.614LDQ-1.012209+1521.502LDQ-0.530409+2291.215LDQ0.662230+1141.037LDQ1.250440-0030.844LDQ1.172249+1851.76LDQ-0.70534-2010.995LDQ1.132251+1130.323LDQ-1.50553-2051.544LDQ-0.132251+1340.673LDQ0.150704+3840.579LDQ0.062314-1160.549LDQ0.050810+3270.842LDQ0.832349+3270.671LDQ-2.10827+1930.658LDQ-0.692353+2830.731LDQ-0.850839+6160.862LDQ-1.792354+1441.81LDQ-0.840903+1690.411LDQ-1.351111+408*0.734LDQ-1.920932+0230.659LDQ0.20017+1542.012LDQ-2.430937+3910.617LDQ-1.560133+207*0.425LDQ-1.080957+0030.907LDQ-0.690229+3411.238LDQ-31015+2770.469LDQ-1.30710+1180.768LDQ-1.841022+1940.828LDQ-0.350758+1431.2LDQ-1.551038+5280.677LDQ1.190802+1031.956LDQ-1.481104+1670.632LDQ0.260833+6541.112LDQ-1.141130+1060.54LDQ0.260835+5801.536LDQ-1.851146+1110.863LDQ-1.180838+1330.684LDQ-0.611156+6310.594LDQ-1.090850+1401.11LDQ-0.951222+2160.435LDQ0.020855+1431.049LDQ-1.951253+1040.824LDQ-0.521040+1231.029LDQ0.161335-0610.625LDQ-1.651100+772*0.311LDQ-0.961415+1720.821LDQ-0.091137+660*0.656LDQ-1.211420+3260.685LDQ1.021241+1660.557LDQ-1.041622+2380.927LDQ-1.472120+1681.805LDQ-1.711732+1601.27LDQ-1.84

注：表3中天体右上角的“*”代表该核占优或瓣占优型射电类星体与表1中的射电类星体相同。

2 统计分析和演化模拟

2.1 红移分布图

图1为Seyfert星系、射电宁静类星体、射电噪类星体红移的分布图，从图1可以得出：Seyfert星系的红移分布在0～0.07的范围；射电宁静类星体的红移分布在0.07～0.3的范围；射电噪类星体的红移分布在0.3～2.4的范围；红移在0.1～0.2的范围内有10个射电噪类星体和射电宁静类星体交叉。

2.2 红移和热光度的关系

图2是红移对热光度的关系图，利用Logistic非线性回归[15-19]的方法分析了射电类星体和Seyfert星系的红移和热光度的相关性，得到了相应的演化曲线，并将Logistic非线性回归分析的结果记录在表4中。从图2和表4可以得出：Logistic非线性回归曲线很好地拟合出红移对热光度关系的演化曲线；射电噪类星体主要分布在演化曲线的右上部分，随着演化的进行，热光度和红移慢慢变小，射电噪类星体演化为射电宁静类星体，当演化进行到一定阶段，射电类星体过渡到Seyfert星系。

图1 红移分布图

图2 红移对热光度

2.3 红移和黑洞质量的关系

图3是红移对黑洞质量的关系图，利用Logistic非线性回归的方法分析了红移对黑洞质量的关系，拟合出相应的演化曲线，并将回归分析的结果记录在表4中，从图2和图3的对比以及表4的结果可以得出红移对热光度与红移对黑洞质量得到的结果是一致的。

2.4 红移和5 GHz射电光度的关系

图4是红移对5 GHz射电光度的关系图，利用Logistic非线性回归的方法分析了红移对5 GHz射电光度的关系，并将结果记录在表4中。从表4可以得到Logistic非线性回归很好地拟合出射电噪类星体到射电宁静类星体的演化曲线。

图3 红移对黑洞质量

图4 红移对5 GHz射电光度

表4 Logistic非线性回归分析结果

注：Logistic非线性回归方程y=A2+(A1-A2)/(1+(x/x0)^n)，r是相关系数，P是置信度水平，N是样品个数。

2.6 红移和核主导参数R的关系

图5 红移对爱丁顿吸积率

图6 红移对和核主导参数R

Fig.6 Core Dominance Parameter (R) values versus redshifts

3 结论和讨论

通过对射电类星体的红移和热光度、黑洞质量、5 GHz射电光度、吸积率的研究得到：(1)射电噪类星体→射电宁静类星体→Seyfert星系的演化，Marecki(2011)也从观测结果支持射电噪类星体→射电宁静类星体的演化[21]，这就验证了射电噪类星体和射电宁静类星体之间本质的不同不是由于指向效应而是一种演化的结果，同时也验证了Punsly(1996)和Park(1988)模型中提出的类星体→Seyfert星系的演化，这可能的解释是具有高红移、高光度、高吸积率的射电噪类星体可能出现在宇宙的早期，随着演化的进行，红移、光度、吸积率慢慢变小，射电噪类星体演化为射电宁静类星体，当演化到一定阶段，吸积的能量不能再维持其吸积过程时，射电类星体开始衰退，当红移达到一定值时，射电类星体过渡到Seyfert星系；(2)核占优型射电类星体和瓣占优型射电类星体的红移与核主导参数R之间没有相关性，这就说明核占优型射电类星体和瓣占优型射电类星体没有明显随红移进行演化。从图6可以得到在LogR>1的射电类星体主要是核占优型类星体，在-0.5

[1]尤莉莎, 张雄. 活动星系核的演化与宇宙学红移[J]. 天文研究与技术——国家天文台台刊, 2007, 4(2): 108-112.

You Lisha, Zhang Xiong. Active galactic nuclei and the redshift[J]. Astronomical Research & Technology——Publications of National Astronomical Observatories of China, 2007, 4(2): 108-112.

[2]Lacy M, Laurent S A, Ridgway S E, et al. The radio luminosity-black hole mass correlation for quasars from the first bright quasar survey and a “unification scheme” for radio-loud and radio-quiet quasars[J]. The Astrophysical Journal, 2001, 551: L17-L21.

[3]McLure R J, Jarvis M J. The relationship between radio luminosity and black hole mass in optically selected quasars[J]. Monthly Notices of the Royal Astronomical Society, 2004, 353(1): L45-L49.

[4]Punsly B. Spectral diagnostics of blazar central engines. II. hydromagnetic theory[J]. The Astrophysical Journal, 1996, 473(1): 178-203.

[5]Park S J, Vishniac E T. The evolution of the central black hole in an active galactic nucleus. I-Evolution with a constant mass influx[J]. The Astrophysical Journal, 1988, 332(1): 135-140.

[6] 鲍玉英, 张雄, 陈洛恩, 等. 活动星系核中黑洞质量和吸积率分布的研究[J]. 天文学报, 2008, 49(2): 123-132.

Bao Yuying, Zhang Xiong, Chen Luoen, et al. Studies of the black hole mass and the eddingtom rate of AGNs[J]. Acta Astronomica Sinica, 2008, 49(2): 123-132.

[7]Zhang L, Cheng K S, Fan J H. The radio and gamma-ray luminosities of blazars[J]. Publications of the Astronomical Society of Japan, 2001, 53: 207-213.

[8]Woo J H, Urry C M. Active galactic nucleus black hole masses and bolometric luminosities[J]. The Astrophysical Journal, 2002, 579(2): 530-544.

[9]Hough D H, Readhead A C S. A complete sample of double-lobed radio quasars for VLBI tests of source models-Definition and statistics[J]. The Astronomical Journal, 1989, 98: 1208-1225.

[10]Hutchings J B, Price R, Gower A C. Radio evolution of quasars at z<1[J]. The Astrophysical Journal, 1988, 329(1): 122-137.

[11]Neff S G, Hutchings J B, Gower A C. Evolution of radio quasars for Z of less than 2[J]. The Astronomical Journal, 1989, 97: 1291-1305.

[12]Murphy D W, Browne I W A, Perley R A. VLA observations of a complete sample of core-dominated radio sources [J]. Monthly Notices of the Royal Astronomical Society,1993, 264(1): 298-318.

[13]Fan J H, Zhang J S. The core dominance parameter of extragalactic radio sources[J]. Astronomy and Astrophysics, 2003, 407(2): 899-904.

[14]Cao X W, Jiang D R. The relation between extended radio and line emission for radio-loud quasars[J]. Monthly Notices of the Royal Astronomical Society, 2001, 320(1): 347-355.

[15]Kellermann K I, Sramek R, Schmidt M, et al. VLA observations of objects in the palomar bright quasar survey[J]. The Astronomical Journal, 1989, 98: 1195-1207.

[16]Cao X W, Jiang D R. Correlation between radio and broad-line emission in radio-loud quasars[J]. Monthly Notices of the Royal Astronomical Society, 1999, 307(2): 802-811.

[17]Drinkwater M J, Webster R L, Francis P J, et al. The parkes half-jansky flat-spectrum sample[J]. Monthly Notices of the Royal Astronomical Society, 1997, 284(1): 85-108.

[18]Feigelson E D, Takashi I, Kembhavi A. Radio and X-ray emission in radio-selected quasars[J]. The Astronomical Journal, 1984, 89: 1464.

[19]唐洁, 吴学兵. 基于Logistic回归模型的Blazar天体的分类[J]. 物理学报, 2011, 60(11): 1-7.

Tang Jie, Wu Xuebing. Classification of Blazar objects based on Logistic regression model[J]. Acta phsyscal Sinica, 2011, 60(11): 1-7.

[20]Orr M J L, Browne I W A. Relativistic beaming and quasar statistics[J]. Monthly Notices of the Royal Astronomical Society, 1982, 200(3): 1067-1080.

[21]Marecki A, Swoboda. The transition from quasar radio-loud to radio-quiet state in the framework of the black hole scalability hypothesis[J]. Astronomy and Astrophysics, 2011, 525(1): 6-14.