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In 1968 Shirley Chisholm became the first Black woman elected to the United States Congress. In 1972 she launched a campaign for the Democratic presidential nomination, breaking another political barrier.
MORE →Reflects the personal views, recollections, and perspective of the author, Mike Davis.
This is a personal recollection on the Move fire on May 13, 1985
| IRAS F11119+3257 | |
|---|---|
 The quasar IRAS F11119+3257 | |
| Observation data (J2000 epoch) | |
| Constellation | Ursa Major |
| Right ascension | 11h 14m 38.91s |
| Declination | +32d 41m 33.34s |
| Redshift | 0.187580 |
| Heliocentric radial velocity | 56,235 km/s |
| Distance | 2.519 Gly (772.3 Mpc) |
| Apparent magnitude (V) | 0.54 |
| Apparent magnitude (B) | 0.43 |
| Surface brightness | 19.2 |
| Characteristics | |
| Type | Sbrst; ULIRG, Sy1 |
| Apparent size (V) | 0.13' x 0.10' |
| Notable features | Luminous infrared galaxy |
| Other designations | |
| B2 1111+32, PGC 34264, F2M J111438.91+324133.29, NVSS J111438+324133, FIRST J111438.9+324133, IVS B1111+329 | |
IRAS F11119+3257 or simply as F11119+3257, is a galaxy located in constellation Ursa Major. With a redshift of 0.187580, it has a light travel time distance of 2.5 billion light-years[1] and is considered an ultraluminous infrared galaxy (ULIRG).[2]
The nucleus of IRAS F11119+3257 is active. It has been classified as a narrow-line Seyfert 1 galaxy[3] and has a post-merger morphology. It is also a categorized as type-1 quasar with fast outflows based on NuSTAR and Suzaku observations.[4] The emission lines that contain high ionization levels are mainly dominated by blueshifted components.[5]
The radio emission of IRAS F11119+3257, is dominated by its active galactic nucleus (AGN).[6] There is an evidence of a central accretion disk.[7] It is also found the galaxy has molecular outflow based on detections of both blue and redshifted wings in the CO(1–0) emission line profile.[7] The estimated molecular mechanical outflow power is around 44.4 ± 0.5 erg s-1, confirming only 2% of the total luminosity has been emitted out by its active galactic nucleus.[8] The central supermassive black hole mass of the galaxy is 2 × 107 solar masses.[9] Apart from the molecular outflows, the galaxy exhibits X-ray emitting winds driven through radiation, suggesting its energy is conserved through quasar-mode feedback.[8][10] Moreover the radio spectrum is peaked at 0.53 ± 0.06 GHz frequencies.[11]
A two-sided radio jet has been discovered in IRAS F11119+3257 based on observations conducted in 2020. The jet is shown to have a separation gap of 200 parsecs in total and is found moving at fast speeds of 0.57c. Evidence also found it is a compact symmetrical object (CSO), depicted as unusual with a measured kinematic age of 6 x 105 years.[11]
Source: Wikipedia. Article content is retrieved live through the MediaWiki API.
IRAS F11119+3257 or simply as F11119+3257, is a galaxy located in constellation Ursa Major. With a redshift of 0.187580, it has a light travel time distance of 2.5 billion light-years and is considered an ultraluminous infrared galaxy (ULIRG).
Chi Ursae Majoris or χ Ursae Majoris, formally named Taiyangshou , is a single star in the northern circumpolar constellation of Ursa Major. The star has an orange hue and is visible to the naked eye at night with an apparent visual magnitude of 3.72. It is located at a distance of approximately 198 light-years from the Sun based on parallax, but is drifting closer with a radial velocity of −9 km/s.
Upsilon Ursae Majoris, Latinized from υ Ursae Majoris, is a binary star in the northern circumpolar constellation of Ursa Major. It is visible to the naked eye with an apparent visual magnitude of +3.79. Based upon an annual parallax shift of 13.24 mas, it is located roughly 246 light-years from the Sun. The primary member of the system, component A, is an F-type subgiant star. It is a Delta Scuti variable with a period of 0.1327 day and an amplitude of 0.050 magnitude. With an estimated age of 1.168 billion years, it is spinning rapidly with a projected rotational velocity of 124.2 km/s and a rotation period of 1.2 days. The star has about 1.57 times the mass of the Sun and 2.79 times the Sun's radius. (De Rosa and colleagues give a mass estimate of 2.2 times the Sun's mass.) It is radiating around 29.5 times the solar luminosity from its outer atmosphere at an effective temperature of 7,211 K. The companion, component B, is a magnitude +11.0 star. As of 2008, it has an angular separation of 11.78 arcseconds along a position angle of 295.4°. This corresponds to a projected separation of 419.8 AU. It has a mass around 40% that of the Sun.
Omega Ursae Majoris (Omega UMa, ω Ursae Majoris, ω UMa) is a binary star system in the northern circumpolar constellation of Ursa Major. It is visible to the naked eye with an apparent visual magnitude of 4.61. Based upon an annual parallax shift of 13.24 mas, it is roughly 246 light years from the Sun. At that distance, the visual magnitude of the star is diminished by an extinction factor of 0.11 due to interstellar dust. This is a single-lined spectroscopic binary star system with an orbital period of 15.8 days and an eccentricity of 0.31. The primary member, component A, is an A-type main sequence star with a stellar classification of A1VsSi:. The stellar spectrum has the appearance of a hot Am star, showing overabundances of many iron-peak and heavier elements, but an underabundance of helium. In particular, it has an abnormal abundance of silicon.
Before the 1921 destruction of Tulsa’s Greenwood District, Black residents had created a remarkable center of business and community life. The district included stores, professional offices, entertainment venues and homes owned by Black citizens. Understanding Greenwood means learning what was built—not only what was burned.
MORE →Madam C.J. Walker
