The Relation of Mid Infrared and Radio Emission in Narrow-Line Seyfert 1 Galaxies

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謝孟哲(Meng-Che Hsieh) 查詢紙本館藏

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天文研究所

論文名稱

(The Relation of Mid Infrared and Radio Emission in Narrow-Line Seyfert 1 Galaxies)

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摘要(中)

我們利用史隆數位巡天計畫(SDSS)、廣域紅外線巡天探測衛星(WISE)、射電暗
源巡天(FIRST) 以及Swift 的X 射線望遠鏡(XRT) 的資料，調查窄線西佛星系的中紅
外線以及電波輻射之間的關係。我們發現窄線西佛星系的中紅外線跟電波輻射之間有
很好的正比關係。另一方面，我們發現中紅外線輻射跟[O III] 譜線強度之間也呈現良
好的正比關係。接著我們發現中紅外線輻射跟黑洞質量也有正比關係。然而我們發現
中紅外線輻射跟X 射線強度似乎並沒有明顯的關聯性。最後我們使用GALFIT 軟體去
將窄線西佛星系分解成核球、星系盤以及活躍星系核三部分。接著我們發現電波輻射
與星系盤亮度的相關性最佳，這或許是恆星形成活動造成的結果。而另一方面，中紅
外線輻射跟[O III] 譜線強度則是來自於活躍星系核。我們的結果顯示窄線西佛星系中
大部分的中紅外線輻射應該是來自於活躍星系核。

摘要(英)

We investigated the relation of mid-infrared (MIR) and radio emission for Narrow-Line
Seyfert 1 (NLSy1) galaxies, using the data from the Sloan Digital Sky Survey (SDSS),
the Wide-Field Infrared Survey Explorer (WISE), the Faint Images of the Radio Sky at
Twenty cm (FIRST), and the Swift X-Ray Telescope (XRT). We found that there is a
positive correlation between the 22m MIR (W4) and the 1.4GHz radio (FIRST) emission.
Besides, the correlation exists between the 22m MIR (W4) and the [O III] emission. Next,
we found that the 22m MIR (W4) is correlated with the black hole mass. However, we
could not find significant correlation between the 22m MIR (W4) and the X-ray emission.
Finally, we utilized a two-dimensional decomposition software, “GALFIT”, to decompose
the NLSy1 galaxies into bulge, disk and AGN components. Then, we found that the radio
emission is well correlated with the disk component brightness for the NLSy1, suggesting
that the radio emission might be related to the star formation activity. Nevertheless, the
MIR and the [O III] emission are related to the AGN. Our results suggest that most of
the MIR emission should be from the central AGN.

關鍵字(中)

★ 活躍星系核
★ 西佛星系

關鍵字(英)

★ AGN
★ Seyfert galaxies

論文目次

Chapter 1 Introduction (p1)
1.1 Active Galactic Nucleus (p1)
1.2 Unification Model (p3)
1.3 Narrow-Line Seyfert 1 Galaxies (p4)
1.4 Supermassive Black Hole Mass (p4)
1.4.1 Correlation of Supermassive Black Hole Mass and Bulge Luminosity (p5)
1.4.2 Correlation of Supermassive Black Hole Mass and Radio Luminosity (p5)
1.5 Emission Mechanism (p6)
1.5.1 Correlation of Far-Infrared and Radio Emission (p6)
1.5.2 Infrared Emission (p6)
1.6 Research Purpose (p6)

Chapter 2 Data and Sample Selection (p7)
2.1 Data (p7)
2.2 Sample Selection (p8)

Chapter 3 Data Reduction and Analysis (p11)
3.1 Luminosity Calculation (p11)
3.1.1 K-correction (p11)
3.1.2 MIR (p12)
3.1.3 Radio (p12)
3.1.4 Optical (p13)
3.1.5 X-Ray (p13)
3.1.6 Conversion of SDSS System into Johnson System (p13)
3.2 X-Ray Spectral Analysis (p14)
3.2.1 XSELECT (p14)
3.2.2 XSPEC (p14)
3.3 Supermassive Black Hole Mass Estimation (p15)
3.4 GALFIT Decomposition (p16)
3.4.1 Fitting Profiles (p16)
3.4.2 Fitting Process(p17)
3.5 Statistical Analysis (p18)
3.5.1 Pearson’s Correlation (p18)
3.5.2 Partial Correlation (p18)

Chapter 4 Results and Discussion (p21)
4.1 The Properties of the Radio and the MIR Emission (p21)
4.2 The Properties of the Ratios of Infrared to Radio Emission (p25)
4.3 The Properties of the [O III] and the MIR Emission (p28)
4.4 The Properties of X-Ray and Multi-Wavelength Emission (p31)
4.5 The Properties of SMBH Mass of NLSy1 (p35)
4.6 The Properties of Galaxy Components of NLSy1 (p38)
4.6.1 Three Components Case (p38)
4.6.2 Two Components Case (p42)
4.6.3 Two Components Case: Radio-loud and Radio-quiet samples (p46)
4.7 Discussion of Mid-Infrared and Radio Emission in NLSy1 Galaxies (p51)
4.8 The Properties of SMBH Mass and Bulge Luminosity (p52)

Chapter 5 Conclusion (p55)

Bibliography (p57)
Appendix (p61)

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指導教授

黃崇源(Chorng-Yuan Hwang)

審核日期

2017-7-20

推文