熊定榮，張 雄，鄭永剛，劉文廣，康 婷，郭 飛

(云南師范大學物理與電子信息學院，云南 昆明 650092)

射電類星體演化的實質(zhì)是指天體在宇宙時標上的變化，而天體的宇宙時標主要與宇宙學紅移有關[1]。在天體演化的過程中，各個階段的宇宙學紅移不同，因此可以根據(jù)宇宙學紅移確定天體的演化。 射電類星體按照射電輻射強度的不同可以分為射電噪類星體(Radio Loud Quasars, RLQ)和射電寧靜類星體(Radio Quiet Quasars, RQQ)[2]，一般用射電噪度(Radio Loudness)等于10來區(qū)分射電寧靜和射電噪類星體；射電噪度大于10稱為射電噪類星體；小于10稱為射電寧靜類星體[3]。然而到底是指向效應還是內(nèi)秉的演化結果造成了射電寧靜和射電噪類星體本質(zhì)的不同，目前還在研究中，這也是構造活動星系核統(tǒng)一結構和演化模型時遇到的最大問題之一。 Punsly(1996)和Park(1988)模型中提出了類星體到Seyfert星系的演化[4-5]，但這一演化一直沒有得到很好的驗證。核占優(yōu)型射電類星體和瓣占優(yōu)型射電類星體之間是否存在演化關系對射電噴流的研究也具有重要意義?；谶@些研究背景，收集和計算了許多射電寧靜類星體、射電噪類星體和Seyfert星系的重要參數(shù)，做出了這些參數(shù)和紅移的關系圖，利用Logistic非線性回歸分析的方法對射電類星體的演化進行擬合，得出相應的演化曲線。

1 樣本選取和數(shù)據(jù)處理

表1 射電類星體樣品

續(xù) 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

續(xù) 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

續(xù) 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星系樣品

續(xù) 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 核占優(yōu)和瓣占優(yōu)型射電類星體樣品

續(xù) 表

NameZ射電形態(tài)logRNameZ射電形態(tài)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中天體右上角的“*”代表該核占優(yōu)或瓣占優(yōu)型射電類星體與表1中的射電類星體相同。

2 統(tǒng)計分析和演化模擬

2.1 紅移分布圖

圖1為Seyfert星系、射電寧靜類星體、射電噪類星體紅移的分布圖，從圖1可以得出：Seyfert星系的紅移分布在0～0.07的范圍；射電寧靜類星體的紅移分布在0.07～0.3的范圍；射電噪類星體的紅移分布在0.3～2.4的范圍；紅移在0.1～0.2的范圍內(nèi)有10個射電噪類星體和射電寧靜類星體交叉。

2.2 紅移和熱光度的關系

圖2是紅移對熱光度的關系圖，利用Logistic非線性回歸[15-19]的方法分析了射電類星體和Seyfert星系的紅移和熱光度的相關性，得到了相應的演化曲線，并將Logistic非線性回歸分析的結果記錄在表4中。從圖2和表4可以得出：Logistic非線性回歸曲線很好地擬合出紅移對熱光度關系的演化曲線；射電噪類星體主要分布在演化曲線的右上部分，隨著演化的進行，熱光度和紅移慢慢變小，射電噪類星體演化為射電寧靜類星體，當演化進行到一定階段，射電類星體過渡到Seyfert星系。

圖1 紅移分布圖

圖2 紅移對熱光度

2.3 紅移和黑洞質(zhì)量的關系

圖3是紅移對黑洞質(zhì)量的關系圖，利用Logistic非線性回歸的方法分析了紅移對黑洞質(zhì)量的關系，擬合出相應的演化曲線，并將回歸分析的結果記錄在表4中，從圖2和圖3的對比以及表4的結果可以得出紅移對熱光度與紅移對黑洞質(zhì)量得到的結果是一致的。

2.4 紅移和5 GHz射電光度的關系

圖4是紅移對5 GHz射電光度的關系圖，利用Logistic非線性回歸的方法分析了紅移對5 GHz射電光度的關系，并將結果記錄在表4中。從表4可以得到Logistic非線性回歸很好地擬合出射電噪類星體到射電寧靜類星體的演化曲線。

圖3 紅移對黑洞質(zhì)量

圖4 紅移對5 GHz射電光度

表4 Logistic非線性回歸分析結果

注：Logistic非線性回歸方程y=A2+(A1-A2)/(1+(x/x0)^n)，r是相關系數(shù)，P是置信度水平，N是樣品個數(shù)。

2.6 紅移和核主導參數(shù)R的關系

圖5 紅移對愛丁頓吸積率

圖6 紅移對和核主導參數(shù)R

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

3 結論和討論

通過對射電類星體的紅移和熱光度、黑洞質(zhì)量、5 GHz射電光度、吸積率的研究得到：(1)射電噪類星體→射電寧靜類星體→Seyfert星系的演化，Marecki(2011)也從觀測結果支持射電噪類星體→射電寧靜類星體的演化[21]，這就驗證了射電噪類星體和射電寧靜類星體之間本質(zhì)的不同不是由于指向效應而是一種演化的結果，同時也驗證了Punsly(1996)和Park(1988)模型中提出的類星體→Seyfert星系的演化，這可能的解釋是具有高紅移、高光度、高吸積率的射電噪類星體可能出現(xiàn)在宇宙的早期，隨著演化的進行，紅移、光度、吸積率慢慢變小，射電噪類星體演化為射電寧靜類星體，當演化到一定階段，吸積的能量不能再維持其吸積過程時，射電類星體開始衰退，當紅移達到一定值時，射電類星體過渡到Seyfert星系；(2)核占優(yōu)型射電類星體和瓣占優(yōu)型射電類星體的紅移與核主導參數(shù)R之間沒有相關性，這就說明核占優(yōu)型射電類星體和瓣占優(yōu)型射電類星體沒有明顯隨紅移進行演化。從圖6可以得到在LogR>1的射電類星體主要是核占優(yōu)型類星體，在-0.5

[1]尤莉莎, 張雄. 活動星系核的演化與宇宙學紅移[J]. 天文研究與技術——國家天文臺臺刊, 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] 鮑玉英, 張雄, 陳洛恩, 等. 活動星系核中黑洞質(zhì)量和吸積率分布的研究[J]. 天文學報, 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]唐潔, 吳學兵. 基于Logistic回歸模型的Blazar天體的分類[J]. 物理學報, 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.