PG 1543+489
PG 1543+489 | |
---|---|
![]() PG 1543+489 captured by SDSS | |
Observation data (J2000.0 epoch) | |
Constellation | Boötes |
Right ascension | 15h 45m 30.24s |
Declination | +48d 46m 09.07s |
Redshift | 0.399824 |
Heliocentric radial velocity | 119,864 km/s |
Distance | 4.559 Gly (1379.8 Mpc) |
Apparent magnitude (V) | 0.051 |
Apparent magnitude (B) | 0.067 |
Surface brightness | 16.5 |
Characteristics | |
Type | Spiral; RQQ, AGN |
Notable features | Luminous infrared galaxy, Seyfert galaxy |
Other designations | |
IRAS F15439+4855, RX J1545.5+4846, PGC 2325245, INTREF 656, 2MASSi J1545302+484609, 2XMM J154530.3+484608, QSO B1544+4855, 1AXG J154530+4845 |
PG 1543+489, also known as QSO B1544+4855 and PGC 2325245, is a quasar located in the constellation of Boötes. At the redshift of 0.399, the object is located 4.5 billion light-years away from Earth.[1] It was first discovered in 1983, by researchers who presented 114 objects in the Palomar-Green bright quasar survey, as one of the best studied samples of active galactic nuclei (AGN).[2]
Characteristics[edit]
PG 1543+489 is classified as a radio-quiet quasar (RQQ) with weak 1.3 mm emission[3][4] and soft X-ray spectra (<Gamma > g = 2.58 +/- 0.05 for z < 0.5).[5] It contains a high X-ray luminosity which it was studied by X-ray satellites like ROSAT[6] and XMM-Newton,[7] who observed its continuum emission is modelled by a power-law component <
The quasar is also classified as a narrow-line Seyfert 1 galaxy,[8][9] a type of AGN that shows all properties of normal Type 1 Seyfert galaxies but has peculiar characteristics such as narrowest Balmer lines with a full width at half-maximum (FWHM) of 1630 km s−1,[10] strong Fe II emission, and extreme properties presented in the X-rays.[11] The measured hard power-law continua in PG 1543+489 is said to have photon indices spanning the range 1.6-2.5 with a mean of 2.1, found only slightly steeper than the norm for 'broad-line' Seyfert 1s. Furthermore, it shows a soft excess typically modelled as blackbody emission (T_bb~100-300eV) that is superposed on the underlying power law.[12] According to data collected from ROSAT, the photon index of the power law is between 2 and 3 for PG 1543+489, with an absorption of cold interstellar gas.[13]
Apart from its Seyfert properties, PG 1543+489 is also classified as an luminous infrared galaxy with its luminosity going up as high as LIR > 1011 L_sun, as observed in the 2-10 keV energy band through new and archival data. According to observations by BeppoSAX, the source in PG 1543+489 is completely Compton thick (N_H > 1025 cm−2).[14]
Observations[edit]
Researchers reanalyzed mid-infrared (5-40
Researchers also found a peculiar feature in PG 1543+489. The quasar shows a blueshift of the [O III] 5007 Å line that is 1150 km s−1 with respect to the systemic velocity of the galaxy as well as the blue asymmetry of its profile.[10] The large [O III] blueshift or so-called 'blue outliers' by researchers, is found theoretically interpreted by the end result of intense outflows whose receding parts are obscured by an optically thick accretion disc[16] or possibly a scenario which the narrow-line region clouds are entrained by decelerating winds, potentially associated with the high Eddington ratio typical of the 'blue outliers'.[17][18]
Absorption system[edit]
Through observations from Hubble Space Telescope, researchers were able to find an absorption-line system at z = 0.07489. Looking at it, they found the sightline passes within
Dampen Lyα absorber[edit]
The Ly
Host galaxy[edit]
The host galaxy of PG 1543+489 is a spiral galaxy[21][22][23] with a gas fraction similar to massive early-type galaxies[24] and an estimated ongoing star formation rate of ~1-250 M⊙ yr−1 according to researchers analyzing 1-500
In additional, the host galaxy has a dusty torus surrounding its AGN whom it contributes significant fraction (~70%) of total infrared (1-1000
According to researchers, the host galaxy is in the midst of a transitional stage between an ultraluminous infrared galaxy and quasar, which the stage normally lasts <~300 Myr.[30] The host galaxy is also found near a companion galaxy with a separation of p' ≃ 2-113 h-1 kpc.[31] With bridge of gas connecting both objects and post-starburst populations, all of this properties suggested a strong interaction between PG 1543+489 and its companion galaxy. In a short period of time, these galaxies will eventually merge.[30]
Black hole[edit]
The supermassive black hole in PG 1543+489 has an estimated solar mass of 1–2.4 × 108M⊙[32] through optical and ultraviolet mass scaling by researchers, with a larger black hole mass expected by using a spectral energy distribution (SED) fitting approach.[7] The black hole is found to grow at a rapid rate[33] with a high Eddington ratio [defined as Lbol/LEdd, where Lbol is the bolometric luminosity and LEdd= (1.3–3.1) × 1046 erg s−1 is the Eddington luminosity] of ≈1.3–3.7 vs ≈2.3,[34] according to researchers who adopted the bolometric correction for quasars.[35] This values are higher as expected compared to previous estimations from the observed 2–10 keV luminosity ≈1.1 × 1044 erg s−1 using the average spectral energy distribution of broad-line quasars which is ≈0.1–0.3.[36]
References[edit]
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