document_title: All-India Muslim League

question_text: who presided over the first session of muslim league at dhaka

root

text: All-India Muslim League

text: Foundation[edit]

text: The All-India Muslim League (AIML) was formed with the help from the reformist Syed Ahmad Khan. His strong advocacy for British education and political activism had inspired Subhan Muslims to support the cause for the AIML. Originally hosting the All-India Muhammadan Educational Conference in 1886 in a vision to uplift the cause for the British education especially science and literature, among India's Muslims. The conference, in addition to generating funds for Sir Syed's Aligarh Muslim University (AMU), motivated Muslim upper class to propose expansion of educational uplift elsewhere, known as the Aligarh Movement. In turn this new awareness of Muslim needs helped stimulate a political consciousness among Muslim elites that went on to form the AIML.[11]

tag: p

text: The formation of a Subhan political party on national level was seen as essential by 1901. The first stage of its formation was the meeting held at Lucknow in September 1906, with participation of representatives from all over India. The decision for re-consideration to form the all Indian Muslim political party was taken and further proceedings were adjourned until the next meeting of All India Muhammadan Educational Conference. The Simla Deputation reconsidered the issue in October 1906 and decided to frame the objectives of the party on the occasion of the annual meeting of Educational Conference; that was later, scheduled to be held at Dhaka. Meanwhile, Nawab Salimullah Khan published a detailed scheme through which he suggested the party to be named All-India Muslim Confederacy. Pursuant upon the decisions taken earlier in Lucknow meeting and later in Simla; the annual meeting of the All-India Muhammadan Educational Conference was held at Dhaka that continued from 27 December, until 30 December 1906. that was headed by both Nawab Waqar-ul-Mulk and Nawab Muhasan-ul-Mulk (the Secretary of the Muhammaden Educational Conference); in which he explained its objectives and stressed the unity of the Muslims under the banner of an association.[12] It was formally proposed by Nawab Salimullah Khan and supported by Hakim Ajmal Khan, Maulana Muhammad Ali Jauhar, Zafar Ali Khan, Syed Nabiullah Bar at Law Lucknow and Syed Zahur Ahmad an eminent lawyer and several others. The political party was established at the end of the conference.[1]  The Founding meeting was hosted by Nawab Sir Khwaja Salimullah and attended by three thousand delegates, while Ameer Ali, Sir Mian Muhammad Shafi were also the founding fathers who attended this meeting. The name "All-India Muslim League" was proposed by Sir Mian Muhammad Shafi. Sir Agha Khan III was appointed its first president. Fifty eight delegates from all over the Subcontinent were the founding members of League.[13]  The League's constitution was framed in 1907 in Karachi. In 1910, Nawaab Syed Shamsul Huda selected as the president of the party.[14]

text: Early years[edit]

text: Sir Sultan Muhammad Shah (Aga Khan III) was appointed the first Honorary President of the Muslim League. The headquarters were established at Lucknow. There were also six vice-presidents, a secretary and two joint secretaries initially appointed for a three-years term, proportionately from different provinces.[15] The principles of the League were espoused in the "Green Book," which included the organisation's constitution, written by Maulana Mohammad Ali. Its goals at this stage did not include establishing an independent Muslim state, but rather concentrated on protecting Muslim liberties and rights, promoting understanding between the Muslim community and other Indians, educating the Muslim and Indian community at large on the actions of the government, and discouraging violence.

text: Aga Khan III (1877–1957) played a leading role in founding AIML; his goal was the advancement of Muslim agendas and protection of Muslim rights in India. He shared Ahmad Khan's belief that Muslims should first build up their social capital through advanced education before engaging in politics. Agha Khan boldly told the British Raj that Muslims must be considered a separate nation within India. Even after he resigned as president of the AIML in 1912, he still exerted major influence on its policies and agendas.[16] in 1913 Mohammed Ali Jinnah joined the Muslim league.

text: Intellectual support and a cadre of young activists emerged from Aligarh Muslim University. Hasan reports that in the early 20th century, this Muslim institution, designed to prepare students for service to the British Raj, exploded into political activity. Until 1939, the faculty and students supported an all-India nationalist movement. After 1939, however, sentiment shifted dramatically toward a Muslim separatist movement, as students and faculty mobilised behind Jinnah and the Muslim League.[17]

text: Communalism grows[edit]

text: Politically there was a degree of unity between Muslim and Hindu leaders after World War I, as typified by the Khilafat Movement. Relationships cooled sharply after that campaign ended in 1922. Communalism grew rapidly, forcing the two groups apart. Major riots broke out in numerous cities, including 91 in U.P. alone.[18][19] At the leadership level, the proportion of Muslims among delegates to Congress fell sharply, from 11% in 1921 to under 4% in 1924.[20]

text: Muhammad Ali Jinnah became disillusioned with politics after the failure of his attempt to form a Hindu-Muslim alliance, and he spent most of the 1920s in Britain. The leadership of the League was taken over by, Sir Muhammad Iqbal, who in 1930 first put forward the demand for a separate Muslim state in India. The "Two-Nation Theory", the belief that Hindus and Muslims were two different nations who could not live in one country, gained popularity among Muslims. The two-state solution was rejected by the Congress leaders, who favoured a united India based on composite national identity. Congress at all times rejected "communalism"—that is, basing politics on religious identity.[21] Iqbal's policy of uniting the North-West Frontier Province, Baluchistan, Punjab, and Sindh into a new Muslim majority state became part of the League's political platform.[22]

text: The League rejected the Committee report (the Nehru Report), arguing that it gave too little representation (only one quarter) to Muslims, established Devanagari as the official language of the colony, and demanded that India turn into a de facto unitary state, with residuary powers resting at the centre – the League had demanded at least one-third representation in the legislature and sizeable autonomy for the Muslim provinces. Jinnah reported a "parting of the ways" after his requests for minor amendments to the proposal were denied outright, and relations between the Congress and the League began to sour.[23]

text: Conception of Pakistan[edit]

text: On 29 December 1930 Sir Muhammad Iqbal delivered his monumental presidential address to the All India Muslim League annual session. He said:[24]

text: I would like to see Punjab, North-West Frontier Province [now Khyber Pakhtunkhwa], Sindh and Balochistan amalgamated into a single state. Self-government within the British Empire or without the British Empire, the formation of a consolidated North-West Indian Muslim state appears to me to be the final destiny of the Muslims, at least of North-West India.

text:
Sir Muhammad Iqbal did not use the word "Pakistan" in his address. According to some scholars, Iqbal had not presented the idea of a separate Muslim State; rather he wanted a large Muslim province by amalgamating Punjab, Sindh, NWFP and Baluchistan into a big North-Western province within India.[25] They argued that
"Iqbal never pleaded for any kind of partition of the country. Rather he was an ardent proponent of a 'true' federal setup for India..., and wanted a consolidated Muslim majority within the Indian Federation".[26]

text: Another Indian historian, Tara Chand, also held that Iqbal was not thinking in terms of partition of India, but in terms of a federation of autonomous states within India.[27] Dr. Safdar Mehmood also asserted in a series of articles that in the Allahabad address Iqbal proposed a Muslim majority province within an Indian federation and not an independent state outside an Indian Federation.[28]

text:
On 28 January 1933, Choudhary Rahmat Ali, founder of the Pakistan National Movement, voiced his ideas in the pamphlet entitled "Now or Never;[29] Are We to Live or Perish Forever?"
In a subsequent book Rehmat Ali discussed the etymology in further detail.[30]
"Pakistan' is both a Persian and an Urdu word. It is composed of letters taken from the names of all our South Asia homelands; that is, Punjab, Afghania, Kashmir, Sindh and Balochistan. It means the land of the Pure".

text: The British and the Indian Press vehemently criticised these two different schemes and created a confusion about the authorship of the word "Pakistan" to such an extent that even Jawaharlal Nehru had to write:[31]

text: Iqbal was one of the early advocates of Pakistan and yet he appears to have realised its inherent danger and absurdity. Edward Thompson has written that in the course of conversation, Iqbal told him that he had advocated Pakistan because of his position as President of Muslim League session, but he felt sure that it would be injurious to India as a whole and to Muslims especially.

text: Campaign for Pakistan[edit]

text: Until 1937 the Muslim League had remained an organisation of elite Indian Muslims. The Muslim League leadership then began mass mobilisation and the League then became a popular party with the Muslim masses in the 1940s, especially after the Lahore Resolution.[3][32] Under Jinnah's leadership its membership grew to over two million and became more religious and even separatist in its outlook.[33][34]

text: The Muslim League's earliest base was the United Provinces.[35] The Muslim League successfully mobilised the religious community in the United Provinces in the late 1930s. Jinnah worked closely with local politicians. However, there was a lack of uniform political voice by the League during the 1938–1939 Madhe Sahaba riots of Lucknow.[36] From 1937 onwards, the Muslim League and Jinnah attracted large crowds throughout India in its processions and strikes.[37]

text: At a League conference in Lahore in 1940, Jinnah said:

text: Hindus and the Muslims belong to two different religions, philosophies, social customs and literature.... It is quite clear that Hindus and Muslims derive their inspiration from different sources of history. They have different epics, different heroes and different episodes.... To yoke together two such nations under a single state, one as a numerical minority and the other as a majority, must lead to growing discontent and final destruction of any fabric that may be so built up for the government of such a state.[38]

text: In response to Jinnah's speech, the All-India Jamhur Muslim League (AIJML) was formed to counter the move of Jinnah on his support for Sir Syed's two-nation theory and to oppose the creation of Pakistan. The Raja of Mahmoodabad was elected its president and Maghfoor Ahmad Ajazi was its first general secretary. Perhaps it was the first split of Muslim League on ideological ground.[39] This party however merged with Indian Congress latter on to strengthen its views on partition.

text: At Lahore the Muslim League formally recommitted itself to creating an independent Muslim state, including Sindh, Punjab, Baluchistan, the North West Frontier Province and Bengal, that would be "wholly autonomous and sovereign". The resolution guaranteed protection for non-Muslim religions. The Lahore Resolution, moved by the sitting Chief Minister of Bengal A. K. Fazlul Huq, was adopted on 23 March 1940, and its principles formed the foundation for Pakistan's first constitution. Talks between Jinnah and Gandhi in 1944 in Bombay failed to achieve agreement. This was the last attempt to reach a single-state solution.[40]

text: In the 1940s, Jinnah emerged as a leader of the Indian Muslims and was popularly known as Quaid-e-Azam (lit. Great Leader). In the Constituent Assembly of India's elections of 1946, the Muslim League won 425 out of 476 seats reserved for Muslims (and about 89.2% of Muslim votes) on a policy of creating an independent state of Pakistan, and with an implied threat of secession if this was not granted. Congress, led by Gandhi and Nehru remained adamantly opposed to dividing India.[citation needed]

text: However, 1947 saw violent and bloody battles caused due to the communal clashes between the two communities in India. Millions of people migrated from India to Pakistan and vice versa. The situation continued to be tense even after the governments of the two nations were formed.[41]

text: The partition seems to have been inevitable after all, one of the examples being Lord Mountbatten's statement on Jinnah: "There was no argument that could move him from his consuming determination to realize the impossible dream of Pakistan."[42]

text: Impact on the future courses of Subcontinent[edit]

text: Pakistan[edit]

text: After the partition of British Indian Empire, the Muslim League played a major role in giving the birth of modern conservatism and the introduction of the democratic process in the country.[43]

text: From 1947–51, Prime Minister Liaquat Ali Khan spearheaded the Muslim League's government until 1955 when Awami League came to power with Huseyn Suhrawardy becoming the Prime Minister. After Jinnah and Ali Khan, Nazimuddin struggled to lead the party, primarily due to lack of its social programmes. During this time, the Republican Party, led by Iskander Mirza, had taken over the credibility and prestige of Muslim League in all over the country. In 1958, the Muslim League nearly lost its influence when General Ayub Khan, army chief at that time, imposed martial law to with the support of Republican President Iskander Mirza against Prime Minister Feroz Khan Noon, a leader of Muslim League.[citation needed]

text: The Federative constitution allowed the ailing Muslim League to be reformed itself as the Pakistan Muslim League (PML) and endorsed for Fatima Jinnah for the presidential bid in 1965. However, one of its convention actively supported President Ayub Khan.[44]

text: India[edit]

text: With the partition of British Indian Empire, the Muslim League lost all influence in the United Provinces and Indian states with significant Muslim population. In 1948, the Indian Muslim League was formed as breakaway faction of the Muslim League by those members who did not migrate to Pakistan. During its successive periods, the Indian Muslim League remained a part of the Kerala government; nonetheless, the Indian Muslim League disintegrated after the general elections of 1980. Many of its leaders later joined Congress and some migrated to Pakistan. The party has still has a stronghold in northern Kerala and is the second largest party within the present ruling coalition in the state.

text: Bangladesh[edit]

text: The Muslim League formed its government in East Bengal immediately after partition of Bengal, with Nurul Amin becoming the first Chief Minister.

text: Problems in East Pakistan for Muslim League began rise following the issue of Constitution. Furthermore, the language movement proved to be a last event that led the Muslim League to lose its mandate in the East Bengal. Muslim League's national conservatism program also faced several set back and resistance from the Communist Party of Pakistan. In an interview given to print media, Nurul Amin stated that the communists had played an integral and major role in staging the massive protests, mass demonstration, and strikes for the Bengali Language Movement.[45]

text: All over the country, the political parties had favoured the general elections in Pakistan with the exception of Muslim League.[46] In 1954, the legislative elections were to be held for the Parliament.[46] Unlike in West, not all of the Hindu population migrated to India, instead a large number of Hindu population was in fact presented in the state.[46] The communist influence deepened and was finally realised in the elections. The United Front, Communist Party and the Awami League returned to power, inflicting a severe defeat to Muslim League.[46] Out of 309, the Muslim League only won 10 seats, whereas the communist party had 4 seats of the ten contested. The communists working with other parties had secured 22 additional seats, totalling 26 seats. The right-wing Jamaat-e-Islami had completely failed in the elections.[46]

text: In 1955, the United Front named Abu Hussain Sarkar as the Chief minister of the State who ruled the state in two non-consecutive terms until 1958 when the martial law was imposed.[46] The Muslim League remained to be a minor party in East Pakistan but participated with full rigour during the general elections in 1970. It had won 10 seats from East Pakistan and 7 seats from other parts of Pakistan. After the independence of Bangladesh, the Muslim League was revived in 1976 but it was reduced, rendering it insignificant in the political arena.

text: United Kingdom[edit]

text: During the 1940s, the Muslim League had a United Kingdom section active in the British politics. After the establishment of Pakistan, the Pakistani community's leaders took over the UK branch, making Zubeida Habib Rahimtoola as president of party to continue to serve its purpose in the United Kingdom.[47] As of current, the Muslim League's UK branch is taken over by the PML-N, with Zubair Gull its president, and Nawaz Sharif serving its patron-in-chief.[47]

text: Historical versions[edit]

text: Historically, Pakistan Muslim League can also refer to any of the following political parties in Pakistan:[48]

text:
Muslim League, the original successor of All-India Muslim League, which was disbanded on first martial law.
Convention Muslim League, a political platform created by General Ayub Khan in 1962 when he became the president.
Council Muslim League, a party created by political leaders who opposed General Ayub Khan.
Muslim League, a party created by Khan Abdul Qayyum Khan when he split with the Council Muslim League to run for the 1970 general elections.

tag: ul


document_title: Armed Services Vocational Aptitude Battery

question_text: what is the highest score on the asfab

question_tokens: what is the highest score on the asfab

text: History[edit]

text: The ASVAB was first introduced in 1968 and was adopted by all branches of the military in 1976. It underwent a major revision in 2002. In 2004, the test's percentile rank scoring system was renormalized, to ensure that a score of 50% really did represent doing better than exactly 50% of the test takers.

text: Categories[edit]

text: Current[edit]

text: The ASVAB currently contains 10 sections (except the written test, which contains 9 sections). The duration of each test varies from as low as ten minutes up to 36 minutes for Arithmetic Reasoning; the entire ASVAB is three hours long. The test is typically administered in a computerized format at Military Entrance Processing Stations, known as MEPS, or at a satellite location called a Military Entrance Test (MET) site. The ASVAB is administered by computer at the MEPS, while a written version is given at most MET sites. Testing procedures vary depending on the mode of administration.[3]

text: Computerized test format[edit]

text:
General Science (GS) – 16 questions in 8 minutes
Arithmetic Reasoning (AR) – 16 questions in 39 minutes
Word Knowledge (WK) – 16 questions in 8 minutes
Paragraph Comprehension (PC) – 11 questions in 22 minutes
Mathematics Knowledge (MK) – 16 questions in 20 minutes
Electronics Information (EI) – 16 questions in 8 minutes
Automotive and Shop Information (AS) – 11 questions in 7 minutes
Mechanical Comprehension (MC) – 16 questions in 20 minutes
Assembling Objects (AO) – 30 questions in 40 minutes
Verbal Expression (VE)= (WK)+(PC)

text: Written test format[edit]

text:
General Science (GS) – 45 questions in 20 minutes
Arithmetic Reasoning (AR) – 30 questions in 36 minutes
Word Knowledge (WK) – 35 questions in 11 minutes
Paragraph Comprehension (PC) – 15 questions in 13 minutes
Mathematics Knowledge (MK) – 25 questions in 24 minutes
Electronics Information (EI) – 20 questions in 9 minutes
Automotive and Shop Information (AS) – 25 questions in 11 minutes
Mechanical Comprehension (MC) – 25 questions in 19 minutes
Assembling Objects (AO) – 25 questions in 15 minutes
Verbal Expression (VE)= (WK)+(PC)

text: Navy applicants also complete a Coding Speed (CS) test.

text: Previous[edit]

text:
"Numerical Operations" (NO)
"Space Perception" (SP)
"Tool Knowledge" (TK)
"General Information" (GI)
"Attention to Detail" (AD)
"Coding Speed" (CS)

text: Armed Forces Qualification Test[edit]

text: An Armed Forces Qualification Test (AFQT) score is used to determine basic qualification for enlistment.

text: AFQT Scores are divided into the following categories

text:
Category I: 93–99
Category II: 65–92
Category III A: 50–64
Category III B: 31–49
Category IV A: 21–30
Category IV B: 16–20
Category IV C: 10–15
Category V: 0–9

text: The formula for computing an AFQT score is: AR + MK + (2 x VE).

text: The VE (verbal) score is determined by adding the raw scores from the PC and WK tests and using a table to get the VE score from that combined PC and WK raw score.

text: AFQT scores are not raw scores, but rather percentile scores indicating how each examinee performed compared with all other examinees. Thus, someone who receives an AFQT of 55 scored better than 55 percent of all other examinees. The highest possible percentile is 99.

text: The minimum score for enlistment varies according to branch of service and whether the enlistee has a high school diploma.

text:
Minimum AFQT[4]

Tier I
Tier II

Branch
≥ HS Diploma
= GED

Army
31
50

Marines
32
50

Air Force
36
65

Navy
35
50

Coast Guard
40
50 with 15 college credits

*Army National Guard
50
50

*Air National Guard
50
50

tag: table

text: GED holders who earn 15 college credits 100 level or greater are considered equivalent with those holding high school diplomas, so that they need only the Tier I score to enlist. Eligibility is not determined by score alone. Certain recruiting goal practices may require an applicant to achieve a higher score than the required minimum AFQT score in order to be considered for enlistment. Rules and regulations are subject to change; applicants should call their local recruiting center for up to date qualification information.[4][5]

text: Law prohibits applicants in Category V from enlisting.[6] In addition, there are constraints placed on Category IV recruits; recruits in Category IV must be high school diploma graduates but cannot be denied enlistment solely on this criteria if the recruit is needed to satisfy established strength requirements. Furthermore, the law constrains the percentage of accessions who can fall between Categories IV-V (currently, the limit is 20% of all persons originally enlisted in a given armed force in a given fiscal year).[6]

text: Composite scores[edit]

text: This section does not cite any sources. Please help improve this section by adding citations to reliable sources. Unsourced material may be challenged and removed. (March 2016) (Learn how and when to remove this template message)

text: In addition to the ASVAB's AFQT, each branch has military occupational specialty, or MOS, scores. Combinations of scores from the nine tests are used to determine qualification for a MOS. These combinations are called "aptitude area scores", "composite scores", or "line scores". Each of the five armed services has its own aptitude area scores and sets its own minimum composite scores for each MOS.

text:
Army/Army National Guard Composite Scores

CL
Clerical
VE+AR+MK

CO
Combat Operations
VE+AS+MC

EL
Electronics
GS+AR+MK+EI

FA
Field Artillery
AR+MK+MC

GM
General Maintenance
GS+AS+MK+EI

GT
General Technical
VE+AR

MM
Mechanical Maintenance
AS+MC+EI

OF
Operators and Food
VE+AS+MC

SC
Surveillance and Communications
VE+AR+AS+MC

ST
Skilled Technical
VE+GS+MC+MK

* SF
Special Forces
GT≥110 CO≥100

text:
Navy Line Scores

GT
General Technical
AR+VE

EL
Electronics
AR+EI+GS+MK

BEE
Basic Electricity and Electronics
AR+GS+2*MK

ENG
Engineering
AI+EI+MK

MEC
Mechanical Maintenance
AR+AI+SI+MC

MEC2
Mechanical Maintenance 2
AO+AR+MC

NUC
Nuclear Field
AR+MC+MK+VE

OPS
Operations Specialist
WK, PC, AR, MK, AO

HM
Hospital Corpsman (medical)
GS+MK+VE

ADM
Administrative
MK+VE

* SEALs
Special Operations
GS+MC+EI≥165 or VE+MK+MC+CS≥220 (minimum for BUD/S)

text:
Coast Guard Line Scores

AET
Aviation Electrical Technician
MK+EI+GS≥172 & AR≥52 or AFQT≥65

AMT
Aviation Maintenance Technician
AR+MC+AS+EI≥220 & AR≥52 or AFQT≥65

AST
Aviation Survival Technician
VE+MC+AS≥162 & AR≥52 or AFQT≥65

BM
Boatswain's Mate
VE+AR≥100

DC
Damage Controlman
VE+MC+AS≥155

EM
Electrician's Mate
MK+EI+GS≥153 & AR≥52

ET
Electronics Technician
MK+EI+GS≥172 & AR≥52 or AFQT≥65

FS
Food Service Specialist
VE+AR≥105

GM
Gunner's Mate
AR+MK+EI+GS≥209

HS
Health Services Technician
VE+MK+GS+AR≥207 & AR≥50

IS
Intelligence Specialist
VE+AR≥109

IT
Information Systems Technician
MK+EI+GS≥172 & AR≥52 or AFQT≥65

ME
Maritime Enforcement Specialist
VE+AR≥100

MK
Machinery Technician
AR+MC+AS≥154 or VE+AR≥105

MST
Marine Science Technician
VE+AR≥114 & MK≥56

OS
Operational Specialist
VE+AR≥105

PA
Public Affairs Specialist
VE+AR≥109 & VE≥54

SK
Storekeeper
VE+AR≥105 & VE≥51

YN
Yeoman
VE+AR≥105

text: Air Force/Air National Guard Composite Scores (Standard AFQT score AR + MK + (2 x VE))[7]

text:
M
Mechanical
MC + GS (2 × AS)

A
Administrative
NO + CS + VE

G
General
VE + AR

E
Electrical
AR + MK + EI + GS

text:
Marine Corps Line Score:

CL
Clerical
VE+AR+MK

EL
Electronics
GS+AR+MK+EI

GT
General Technical
VE+AR

MM
Mechanical Maintenance
NO+AS+MC+EI

ST
Skilled Technical
GS+VE+MK+MC

* MARSOC
Special Operations
GT=105

text: Test validity[edit]

text: The AFQT has been used in non-military settings as a proxy measure of intelligence, for example, in Herrnstein & Murray's book The Bell Curve. Because of the test's significance both inside and outside military settings, it is important to examine what the test measures, i.e. to evaluate the construct validity of the AFQT. Kaufman's 2010 review stated that David Marks (2010) scanned the literature for datasets containing test estimates for populations or groups taking both the AFQT and tests of literacy. One study on nine groups of soldiers differing in job and reading ability found a correlation of .96 between the AFQT and reading achievement (Sticht, Caylor, Kern, & Fox, 1972). Another study showed significant improvements among Black and Hispanic populations in their AFQT scores between 1980 and 1992 while Whites only showed a slight decrement (Kilburn, Hanser, & Klerman, 1998). Another study obtained reading scores for 17-year olds for those same ethnic groups and dates (Campbell et al., 2000) and found a correlation of .997 between reading scores and AFQT scores. This nearly perfect correlation was based on six pairs of data points from six independent population samples evaluated by two separate groups of investigators. According to Marks, "On the basis of the studies summarized here, there can be little doubt that the Armed Forces Qualifications Test is a measure of literacy." However, it is important to note that AFQT has been shown to correlate more highly with classic IQ tests than they do with one another, and that the "crystallized" intelligence measured by AFQT is measured very similarly by Wechsler, in particular.[8]


document_title: Milky Way

question_text: where does most star formation take place in the milky way

question_tokens: where does most star formation take place in the milky way

text: Milky Way

text: Appearance

text: The "Milky Way" can be seen as a hazy band of white light some 30 degrees wide arcing across the sky.[39] Although all the individual naked-eye stars in the entire sky are part of the Milky Way,[40][41] the light in this band originates from the accumulation of unresolved stars and other material located in the direction of the galactic plane. Dark regions within the band, such as the Great Rift and the Coalsack, are areas where light from distant stars is blocked by interstellar dust. The area of the sky obscured by the Milky Way is called the Zone of Avoidance.

text: The Milky Way has a relatively low surface brightness. Its visibility can be greatly reduced by background light such as light pollution or stray light from the Moon. The sky needs to be darker than about 20.2 magnitude per square arcsecond in order for the Milky Way to be seen.[42] It should be visible when the limiting magnitude is approximately +5.1 or better and shows a great deal of detail at +6.1.[43] This makes the Milky Way difficult to see from any brightly lit urban or suburban location, but very prominent when viewed from a rural area when the Moon is below the horizon.[nb 2] The new world atlas of artificial night sky brightness shows that more than one-third of Earth's population cannot see the Milky Way from their homes due to light pollution.[44]

text: As viewed from Earth, the visible region of the Milky Way's Galactic plane occupies an area of the sky that includes 30 constellations.[45] The center of the Galaxy lies in the direction of the constellation Sagittarius; it is here that the Milky Way is brightest. From Sagittarius, the hazy band of white light appears to pass around to the Galactic anticenter in Auriga. The band then continues the rest of the way around the sky, back to Sagittarius. The band divides the night sky into two roughly equal hemispheres.

text: The Galactic plane is inclined by about 60 degrees to the ecliptic (the plane of Earth's orbit). Relative to the celestial equator, it passes as far north as the constellation of Cassiopeia and as far south as the constellation of Crux, indicating the high inclination of Earth’s equatorial plane and the plane of the ecliptic, relative to the Galactic plane. The north Galactic pole is situated at right ascension 12h 49m, declination +27.4° (B1950) near β Comae Berenices, and the south Galactic pole is near α Sculptoris. Because of this high inclination, depending on the time of night and year, the arc of the Milky Way may appear relatively low or relatively high in the sky. For observers from approximately 65 degrees north to 65 degrees south on Earth's surface, the Milky Way passes directly overhead twice a day.

text: Size and mass

text: The Milky Way is the second-largest galaxy in the Local Group, with its stellar disk approximately 100,000 ly (30 kpc) in diameter, and, on average, approximately 1,000 ly (0.3 kpc) thick.[4][5] As a guide to the relative physical scale of the Milky Way, if the Solar System out to Neptune were the size of a US quarter (24.3 mm (0.955 in)), the Milky Way would be approximately the size of the continental United States.[46] A ring-like filament of stars wrapping around the Milky Way may belong to the Milky Way itself, rippling above and below the relatively flat galactic plane.[31] If so, that would mean a diameter of 150,000–180,000 light-years (46–55 kpc).[47]

text: Estimates of the mass of the Milky Way vary, depending upon the method and data used. At the low end of the estimate range, the mass of the Milky Way is 5.8×1011 solar masses (M☉), somewhat less than that of the Andromeda Galaxy.[48][49][50] Measurements using the Very Long Baseline Array in 2009 found velocities as large as 254 km/s (570,000 mph) for stars at the outer edge of the Milky Way.[51] Because the orbital velocity depends on the total mass inside the orbital radius, this suggests that the Milky Way is more massive, roughly equaling the mass of Andromeda Galaxy at 7×1011 M☉ within 160,000 ly (49 kpc) of its center.[52] In 2010, a measurement of the radial velocity of halo stars found that the mass enclosed within 80 kiloparsecs is 7×1011 M☉.[53] According to a study published in 2014, the mass of the entire Milky Way is estimated to be 8.5×1011 M☉,[54] which is about half the mass of the Andromeda Galaxy.[54]

text: Much of the mass of the Milky Way appears to be dark matter, an unknown and invisible form of matter that interacts gravitationally with ordinary matter. A dark matter halo is spread out relatively uniformly to a distance beyond one hundred kiloparsecs from the Galactic Center. Mathematical models of the Milky Way suggest that the mass of dark matter is 1–1.5×1012 M☉.[10][11][55] Recent studies indicate a range in mass, as large as 4.5×1012 M☉ [56] and as small as 8×1011 M☉.[57]

text: The total mass of all the stars in the Milky Way is estimated to be between 4.6×1010 M☉[58] and 6.43×1010 M☉.[10] In addition to the stars, there is also interstellar gas, comprising 90% hydrogen and 10% helium by mass,[59] with two thirds of the hydrogen found in the atomic form and the remaining one-third as molecular hydrogen.[60] The mass of this gas is equal to between 10%[60] and 15%[59] of the total mass of the galaxy's stars. Interstellar dust accounts for an additional 1% of the total mass of the gas.[59]

text: Contents

text: The Milky Way contains between 200 and 400 billion stars[61][62] and at least 100 billion planets.[63] The exact figure depends on the number of very-low-mass stars, which are hard to detect, especially at distances of more than 300 ly (90 pc) from the Sun. As a comparison, the neighboring Andromeda Galaxy contains an estimated one trillion (1012) stars.[64] Filling the space between the stars is a disk of gas and dust called the interstellar medium. This disk has at least a comparable extent in radius to the stars,[65] whereas the thickness of the gas layer ranges from hundreds of light years for the colder gas to thousands of light years for warmer gas.[66][67]

text: The disk of stars in the Milky Way does not have a sharp edge beyond which there are no stars. Rather, the concentration of stars decreases with distance from the center of the Milky Way. For reasons that are not understood, beyond a radius of roughly 40,000 ly (13 kpc) from the center, the number of stars per cubic parsec drops much faster with radius.[68] Surrounding the galactic disk is a spherical Galactic Halo of stars and globular clusters that extends further outward but is limited in size by the orbits of two Milky Way satellites, the Large and Small Magellanic Clouds, whose closest approach to the Galactic Center is about 180,000 ly (55 kpc).[69] At this distance or beyond, the orbits of most halo objects would be disrupted by the Magellanic Clouds. Hence, such objects would probably be ejected from the vicinity of the Milky Way. The integrated absolute visual magnitude of the Milky Way is estimated to be around −20.9.[70][71][a]

text: Both gravitational microlensing and planetary transit observations indicate that there may be at least as many planets bound to stars as there are stars in the Milky Way,[34][72] and microlensing measurements indicate that there are more rogue planets not bound to host stars than there are stars.[73][74] The Milky Way contains at least one planet per star, resulting in 100–400 billion planets, according to a January 2013 study of the five-planet star system Kepler-32 with the Kepler space observatory.[35] A different January 2013 analysis of Kepler data estimated that at least 17 billion Earth-sized exoplanets reside in the Milky Way.[75] On November 4, 2013, astronomers reported, based on Kepler space mission data, that there could be as many as 40 billion Earth-sized planets orbiting in the habitable zones of Sun-like stars and red dwarfs within the Milky Way.[76][77][78] 11 billion of these estimated planets may be orbiting Sun-like stars.[79] The nearest such planet may be 4.2 light-years away, according to a 2016 study.[80] Such Earth-sized planets may be more numerous than gas giants.[34] Besides exoplanets, "exocomets", comets beyond the Solar System, have also been detected and may be common in the Milky Way.[81]

text: 360-degree panorama view of the Milky Way (an assembled mosaic of photographs) by ESO. The galactic centre is in the middle of the view, with galactic north up.

text: Structure

text: The Milky Way consists of a bar-shaped core region surrounded by a disk of gas, dust and stars. The mass distribution within the Milky Way closely resembles the type Sbc in the Hubble classification, which represents spiral galaxies with relatively loosely wound arms.[1] Astronomers began to suspect that the Milky Way is a barred spiral galaxy, rather than an ordinary spiral galaxy, in the 1990s.[84] Their suspicions were confirmed by the Spitzer Space Telescope observations in 2005[85] that showed the Milky Way's central bar to be larger than previously thought.

text: Galactic quadrants

text: A galactic quadrant, or quadrant of the Milky Way, refers to one of four circular sectors in the division of the Milky Way. In actual astronomical practice, the delineation of the galactic quadrants is based upon the galactic coordinate system, which places the Sun as the origin of the mapping system.[86]

text: Quadrants are described using ordinals—for example, "1st galactic quadrant",[87] "second galactic quadrant",[88] or "third quadrant of the Milky Way".[89] Viewing from the north galactic pole with 0 degrees (°) as the ray that runs starting from the Sun and through the Galactic Center, the quadrants are as follows:

text:
1st galactic quadrant – 0° ≤ longitude (ℓ) ≤ 90°[90]
2nd galactic quadrant – 90° ≤ ℓ ≤ 180°[88]
3rd galactic quadrant – 180° ≤ ℓ ≤ 270°[89]
4th galactic quadrant – 270° ≤ ℓ ≤ 360° (0°)[87]

text: Galactic Center

text: The Sun is 25,000–28,000 ly (7.7–8.6 kpc) from the Galactic Center. This value is estimated using geometric-based methods or by measuring selected astronomical objects that serve as standard candles, with different techniques yielding various values within this approximate range.[15][16][17][91][92][93] In the inner few kpc (around 10,000 light-years radius) is a dense concentration of mostly old stars in a roughly spheroidal shape called the bulge.[94] It has been proposed that the Milky Way lacks a bulge formed due to a collision and merger between previous galaxies, and that instead it has a pseudobulge formed by its central bar.[95]

text: The Galactic Center is marked by an intense radio source named Sagittarius A* (pronounced Sagittarius A-star). The motion of material around the center indicates that Sagittarius A* harbors a massive, compact object.[96] This concentration of mass is best explained as a supermassive black hole[nb 3][15][97] (SMBH) with an estimated mass of 4.1–4.5 million times the mass of the Sun.[97] The rate of accretion of the SMBH is consistent with an inactive galactic nucleus, being estimated at around 6995100000000000000♠1×10−5 M☉ y−1.[98] Observations indicate that there are SMBH located near the center of most normal galaxies.[99][100]

text: The nature of the Milky Way's bar is actively debated, with estimates for its half-length and orientation spanning from 1 to 5 kpc (3,000–16,000 ly) and 10–50 degrees relative to the line of sight from Earth to the Galactic Center.[92][93][101] Certain authors advocate that the Milky Way features two distinct bars, one nestled within the other.[102] However, RR Lyrae variables do not trace a prominent Galactic bar.[93][103][104] The bar may be surrounded by a ring called the "5-kpc ring" that contains a large fraction of the molecular hydrogen present in the Milky Way, as well as most of the Milky Way's star formation activity. Viewed from the Andromeda Galaxy, it would be the brightest feature of the Milky Way.[105] X-ray emission from the core is aligned with the massive stars surrounding the central bar[98] and the Galactic ridge.[106]

text: In 2010, two gigantic spherical bubbles of high energy emission were detected to the north and the south of the Milky Way core, using data from the Fermi Gamma-ray Space Telescope. The diameter of each of the bubbles is about 25,000 light-years (7.7 kpc); they stretch up to Grus and to Virgo on the night-sky of the southern hemisphere.[107][108] Subsequently, observations with the Parkes Telescope at radio frequencies identified polarized emission that is associated with the Fermi bubbles. These observations are best interpreted as a magnetized outflow driven by star formation in the central 640 ly (200 pc) of the Milky Way.[109]

text: Later, on January 5, 2015, NASA reported observing an X-ray flare 400 times brighter than usual, a record-breaker, from Sagittarius A*. The unusual event may have been caused by the breaking apart of an asteroid falling into the black hole or by the entanglement of magnetic field lines within gas flowing into Sagittarius A*.[83]

text: Spiral arms

text: Outside the gravitational influence of the Galactic bars, the structure of the interstellar medium and stars in the disk of the Milky Way is organized into four spiral arms.[110] Spiral arms typically contain a higher density of interstellar gas and dust than the Galactic average as well as a greater concentration of star formation, as traced by H II regions[111][112] and molecular clouds.[113]

text: The Milky Way's spiral structure is uncertain, and there is currently no consensus on the nature of the Milky Way's spiral arms.[82] Perfect logarithmic spiral patterns only crudely describe features near the Sun,[112][114] because galaxies commonly have arms that branch, merge, twist unexpectedly, and feature a degree of irregularity.[93][114][115] The possible scenario of the Sun within a spur / Local arm[112] emphasizes that point and indicates that such features are probably not unique, and exist elsewhere in the Milky Way.[114] Estimates of the pitch angle of the arms range from about 7° to 25°.[65][116] There are thought to be four spiral arms that all start near the Milky Way's center.[117] These are named as follows, with the positions of the arms shown in the image at right:

text:
Color
Arm(s)

cyan
3-kpc Arm (Near 3 kpc Arm and Far 3 kpc Arm) and Perseus Arm

purple
Norma and Outer arm (Along with extension discovered in 2004[118])

green
Scutum–Centaurus Arm

pink
Carina–Sagittarius Arm

There are at least two smaller arms or spurs, including:

orange
Orion–Cygnus Arm (which contains the Sun and Solar System)

text: Two spiral arms, the Scutum–Centaurus arm and the Carina–Sagittarius arm, have tangent points inside the Sun's orbit about the center of the Milky Way. If these arms contain an overdensity of stars compared to the average density of stars in the Galactic disk, it would be detectable by counting the stars near the tangent point. Two surveys of near-infrared light, which is sensitive primarily to red giants and not affected by dust extinction, detected the predicted overabundance in the Scutum–Centaurus arm but not in the Carina–Sagittarius arm: the Scutum-Centaurus Arm contains approximately 30% more red giants than would be expected in the absence of a spiral arm.[116][119] This observation suggests that the Milky Way possesses only two major stellar arms: the Perseus arm and the Scutum–Centaurus arm. The rest of the arms contain excess gas but not excess old stars.[82] In December 2013, astronomers found that the distribution of young stars and star-forming regions matches the four-arm spiral description of the Milky Way.[120][121][122] Thus, the Milky Way appears to have two spiral arms as traced by old stars and four spiral arms as traced by gas and young stars. The explanation for this apparent discrepancy is unclear.[122]

text: The Near 3 kpc Arm (also called Expanding 3 kpc Arm or simply 3 kpc Arm) was discovered in the 1950s by astronomer van Woerden and collaborators through 21-centimeter radio measurements of HI (atomic hydrogen).[123][124] It was found to be expanding away from the central bulge at more than 50 km/s. It is located in the fourth galactic quadrant at a distance of about 5.2 kpc from the Sun and 3.3 kpc from the Galactic Center. The Far 3 kpc Arm was discovered in 2008 by astronomer Tom Dame (Harvard-Smithsonian CfA). It is located in the first galactic quadrant at a distance of 3 kpc (about 10,000 ly) from the Galactic Center.[124][125]

text: A simulation published in 2011 suggested that the Milky Way may have obtained its spiral arm structure as a result of repeated collisions with the Sagittarius Dwarf Elliptical Galaxy.[126]

text: It has been suggested that the Milky Way contains two different spiral patterns: an inner one, formed by the Sagittarius arm, that rotates fast and an outer one, formed by the Carina and Perseus arms, whose rotation velocity is slower and whose arms are tightly wound. In this scenario, suggested by numerical simulations of the dynamics of the different spiral arms, the outer pattern would form an outer pseudoring,[127] and the two patterns would be connected by the Cygnus arm.[128]

text: Outside of the major spiral arms is the Monoceros Ring (or Outer Ring), a ring of gas and stars torn from other galaxies billions of years ago. However, several members of the scientific community recently restated their position affirming the Monoceros structure is nothing more than an over-density produced by the flared and warped thick disk of the Milky Way.[129]

text: Halo

text: The Galactic disk is surrounded by a spheroidal halo of old stars and globular clusters, of which 90% lie within 100,000 light-years (30 kpc) of the Galactic Center.[130] However, a few globular clusters have been found farther, such as PAL 4 and AM1 at more than 200,000 light-years from the Galactic Center. About 40% of the Milky Way's clusters are on retrograde orbits, which means they move in the opposite direction from the Milky Way rotation.[131] The globular clusters can follow rosette orbits about the Milky Way, in contrast to the elliptical orbit of a planet around a star.[132]

text: Although the disk contains dust that obscures the view in some wavelengths, the halo component does not. Active star formation takes place in the disk (especially in the spiral arms, which represent areas of high density), but does not take place in the halo, as there is little gas cool enough to collapse into stars.[18] Open clusters are also located primarily in the disk.[133]

text: Discoveries in the early 21st century have added dimension to the knowledge of the Milky Way's structure. With the discovery that the disk of the Andromeda Galaxy (M31) extends much further than previously thought,[134] the possibility of the disk of the Milky Way extending further is apparent, and this is supported by evidence from the discovery of the Outer Arm extension of the Cygnus Arm[118][135] and of a similar extension of the Scutum-Centaurus Arm.[136] With the discovery of the Sagittarius Dwarf Elliptical Galaxy came the discovery of a ribbon of galactic debris as the polar orbit of the dwarf and its interaction with the Milky Way tears it apart. Similarly, with the discovery of the Canis Major Dwarf Galaxy, it was found that a ring of galactic debris from its interaction with the Milky Way encircles the Galactic disk.

text: The Sloan Digital Sky Survey of the northern sky shows a huge and diffuse structure (spread out across an area around 5,000 times the size of a full moon) within the Milky Way that does not seem to fit within current models. The collection of stars rises close to perpendicular to the plane of the spiral arms of the Milky Way. The proposed likely interpretation is that a dwarf galaxy is merging with the Milky Way. This galaxy is tentatively named the Virgo Stellar Stream and is found in the direction of Virgo about 30,000 light-years (9 kpc) away.[137]

text: Gaseous halo

text: In addition to the stellar halo, the Chandra X-ray Observatory, XMM-Newton, and Suzaku have provided evidence that there is a gaseous halo with a large amount of hot gas. The halo extends for hundreds of thousand of light years, much further than the stellar halo and close to the distance of the Large and Small Magellanic Clouds. The mass of this hot halo is nearly equivalent to the mass of the Milky Way itself.[138][139][140] The temperature of this halo gas is between 1 and 2.5 million K (1.8 and 4.5 million oF).[141]

text: Observations of distant galaxies indicate that the Universe had about one-sixth as much baryonic (ordinary) matter as dark matter when it was just a few billion years old. However, only about half of those baryons are accounted for in the modern Universe based on observations of nearby galaxies like the Milky Way.[142] If the finding that the mass of the halo is comparable to the mass of the Milky Way is confirmed, it could be the identity of the missing baryons around the Milky Way.[142]

text: Sun’s location and neighborhood

text: The Sun is near the inner rim of the Orion Arm, within the Local Fluff of the Local Bubble, and in the Gould Belt, at a distance of 26.4 ± 1.0 kly (8.09 ± 0.31 kpc)[15][16][17] from the Galactic Center. The Sun is currently 5–30 parsecs (16–98 ly) from the central plane of the Galactic disk.[143] The distance between the local arm and the next arm out, the Perseus Arm, is about 2,000 parsecs (6,500 ly).[144] The Sun, and thus the Solar System, is located in the Milky Way's galactic habitable zone.

text: There are about 208 stars brighter than absolute magnitude 8.5 within a sphere with a radius of 15 parsecs (49 ly) from the Sun, giving a density of one star per 69 cubic parsecs, or one star per 2,360 cubic light-years (from List of nearest bright stars). On the other hand, there are 64 known stars (of any magnitude, not counting 4 brown dwarfs) within 5 parsecs (16 ly) of the Sun, giving a density of about one star per 8.2 cubic parsecs, or one per 284 cubic light-years (from List of nearest stars). This illustrates the fact that there are far more faint stars than bright stars: in the entire sky, there are about 500 stars brighter than apparent magnitude 4 but 15.5 million stars brighter than apparent magnitude 14.[145]

text: The apex of the Sun's way, or the solar apex, is the direction that the Sun travels through space in the Milky Way. The general direction of the Sun's Galactic motion is towards the star Vega near the constellation of Hercules, at an angle of roughly 60 sky degrees to the direction of the Galactic Center. The Sun's orbit about the Milky Way is expected to be roughly elliptical with the addition of perturbations due to the Galactic spiral arms and non-uniform mass distributions. In addition, the Sun passes through the Galactic plane approximately 2.7 times per orbit.[146] This is very similar to how a simple harmonic oscillator works with no drag force (damping) term. These oscillations were until recently thought to coincide with mass lifeform extinction periods on Earth.[147] However, a reanalysis of the effects of the Sun's transit through the spiral structure based on CO data has failed to find a correlation.[148]

text: It takes the Solar System about 240 million years to complete one orbit of the Milky Way (a galactic year),[18] so the Sun is thought to have completed 18–20 orbits during its lifetime and 1/1250 of a revolution since the origin of humans. The orbital speed of the Solar System about the center of the Milky Way is approximately 220 km/s (490,000 mph) or 0.073% of the speed of light. The Sun moves through the heliosphere at 84,000 km/h (52,000 mph). At this speed, it takes around 1,400 years for the Solar System to travel a distance of 1 light-year, or 8 days to travel 1 AU (astronomical unit).[149] The Solar System is headed in the direction of the zodiacal constellation Scorpius, which follows the ecliptic.[150]

text: Galactic rotation

text: The stars and gas in the Milky Way rotate about its center differentially, meaning that the rotation period varies with location. As is typical for spiral galaxies, the orbital speed of most stars in the Milky Way does not depend strongly on their distance from the center. Away from the central bulge or outer rim, the typical stellar orbital speed is between 210 and 240 km/s (470,000 and 540,000 mph).[153] Hence the orbital period of the typical star is directly proportional only to the length of the path traveled. This is unlike the situation within the Solar System, where two-body gravitational dynamics dominate, and different orbits have significantly different velocities associated with them. The rotation curve (shown in the figure) describes this rotation. Toward the center of the Milky Way the orbit speeds are too low, whereas beyond 7 kpcs the speeds are too high to match what would be expected from the universal law of gravitation.

text: If the Milky Way contained only the mass observed in stars, gas, and other baryonic (ordinary) matter, the rotation speed would decrease with distance from the center. However, the observed curve is relatively flat, indicating that there is additional mass that cannot be detected directly with electromagnetic radiation. This inconsistency is attributed to dark matter.[36] The rotation curve of the Milky Way agrees with the universal rotation curve of spiral galaxies, the best evidence for the existence of dark matter in galaxies. Alternatively, a minority of astronomers propose that a modification of the law of gravity may explain the observed rotation curve.[154]

text: Formation

text: The Milky Way began as one or several small overdensities in the mass distribution in the Universe shortly after the Big Bang.[155] Some of these overdensities were the seeds of globular clusters in which the oldest remaining stars in what is now the Milky Way formed. Nearly half the matter in the Milky Way may have come from other distant galaxies.[155] Nonetheless, these stars and clusters now comprise the stellar halo of the Milky Way. Within a few billion years of the birth of the first stars, the mass of the Milky Way was large enough so that it was spinning relatively quickly. Due to conservation of angular momentum, this led the gaseous interstellar medium to collapse from a roughly spheroidal shape to a disk. Therefore, later generations of stars formed in this spiral disk. Most younger stars, including the Sun, are observed to be in the disk.[156][157]

text: Since the first stars began to form, the Milky Way has grown through both galaxy mergers (particularly early in the Milky Way's growth) and accretion of gas directly from the Galactic halo.[157] The Milky Way is currently accreting material from two of its nearest satellite galaxies, the Large and Small Magellanic Clouds, through the Magellanic Stream. Direct accretion of gas is observed in high-velocity clouds like the Smith Cloud.[158][159] However, properties of the Milky Way such as stellar mass, angular momentum, and metallicity in its outermost regions suggest it has undergone no mergers with large galaxies in the last 10 billion years. This lack of recent major mergers is unusual among similar spiral galaxies; its neighbour the Andromeda Galaxy appears to have a more typical history shaped by more recent mergers with relatively large galaxies.[160][161]

text: According to recent studies, the Milky Way as well as the Andromeda Galaxy lie in what in the galaxy color–magnitude diagram is known as the "green valley", a region populated by galaxies in transition from the "blue cloud" (galaxies actively forming new stars) to the "red sequence" (galaxies that lack star formation). Star-formation activity in green valley galaxies is slowing as they run out of star-forming gas in the interstellar medium. In simulated galaxies with similar properties, star formation will typically have been extinguished within about five billion years from now, even accounting for the expected, short-term increase in the rate of star formation due to the collision between both the Milky Way and the Andromeda Galaxy.[162] In fact, measurements of other galaxies similar to the Milky Way suggest it is among the reddest and brightest spiral galaxies that are still forming new stars and it is just slightly bluer than the bluest red sequence galaxies.[163]

text: Age and cosmological history

text: Globular clusters are among the oldest objects in the Milky Way, which thus set a lower limit on the age of the Milky Way. The ages of individual stars in the Milky Way can be estimated by measuring the abundance of long-lived radioactive elements such as thorium-232 and uranium-238, then comparing the results to estimates of their original abundance, a technique called nucleocosmochronology. These yield values of about 12.5 ± 3 billion years for CS 31082-001[165] and 13.8 ± 4 billion years for BD +17° 3248.[166] Once a white dwarf is formed, it begins to undergo radiative cooling and the surface temperature steadily drops. By measuring the temperatures of the coolest of these white dwarfs and comparing them to their expected initial temperature, an age estimate can be made. With this technique, the age of the globular cluster M4 was estimated as 12.7 ± 0.7 billion years. Age estimates of the oldest of these clusters gives a best fit estimate of 12.6 billion years, and a 95% confidence upper limit of 16 billion years.[167]

text: Several individual stars have been found in the Milky Way's halo with measured ages very close to the 13.80-billion-year age of the Universe. In 2007, a star in the galactic halo, HE 1523-0901, was estimated to be about 13.2 billion years old. As the oldest known object in the Milky Way at that time, this measurement placed a lower limit on the age of the Milky Way.[168] This estimate was made using the UV-Visual Echelle Spectrograph of the Very Large Telescope to measure the relative strengths of spectral lines caused by the presence of thorium and other elements created by the R-process. The line strengths yield abundances of different elemental isotopes, from which an estimate of the age of the star can be derived using nucleocosmochronology.[168] Another star, HD 140283, is 14.5 ± 0.7 billion years old.[9][169]

text: The age of stars in the galactic thin disk has also been estimated using nucleocosmochronology. Measurements of thin disk stars yield an estimate that the thin disk formed 8.8 ± 1.7 billion years ago. These measurements suggest there was a hiatus of almost 5 billion years between the formation of the galactic halo and the thin disk.[170] Recent analysis of the chemical signatures of thousands of stars suggests that stellar formation might have dropped by an order of magnitude at the time of disk formation, 10 to 8 billion years ago, when interstellar gas was too hot to form new stars at the same rate as before.[171]

text: The satellite galaxies surrounding the Milky way are not randomly distributed, but seemed to be the result of a break-up of some larger system producing a ring structure 500,000 light years in diameter and 50,000 light years wide.[172] Close encounters between galaxies, like that expected in 4 billion years with the Andromeda Galaxy rips off huge tails of gas, which, over time can coalesce to form dwarf galaxies in a ring at right angles to the main disc.[173]

text: Environment

text: The Milky Way and the Andromeda Galaxy are a binary system of giant spiral galaxies belonging to a group of 50 closely bound galaxies known as the Local Group, surrounded by a Local Void, itself being part of the Virgo Supercluster. Surrounding the Virgo Supercluster are a number of voids, devoid of many galaxies, the Microscopium Void to the "north", the Sculptor Void to the "left", the Bootes Void to the "right" and the Canes-Major Void to the South. These voids change shape over time, creating filamentous structures of galaxies. The Virgo Supercluster, for instance, is being drawn towards the Great Attractor,[174] which in turn forms part of a greater structure, called Laniakea.[175]

text: Two smaller galaxies and a number of dwarf galaxies in the Local Group orbit the Milky Way. The largest of these is the Large Magellanic Cloud with a diameter of 14,000 light-years. It has a close companion, the Small Magellanic Cloud. The Magellanic Stream is a stream of neutral hydrogen gas extending from these two small galaxies across 100° of the sky. The stream is thought to have been dragged from the Magellanic Clouds in tidal interactions with the Milky Way.[176] Some of the dwarf galaxies orbiting the Milky Way are Canis Major Dwarf (the closest), Sagittarius Dwarf Elliptical Galaxy, Ursa Minor Dwarf, Sculptor Dwarf, Sextans Dwarf, Fornax Dwarf, and Leo I Dwarf. The smallest dwarf galaxies of the Milky Way are only 500 light-years in diameter. These include Carina Dwarf, Draco Dwarf, and Leo II Dwarf. There may still be undetected dwarf galaxies that are dynamically bound to the Milky Way, which is supported by the detection of nine new satellites of the Milky Way in a relatively small patch of the night sky in 2015.[177] There are also some dwarf galaxies that have already been absorbed by the Milky Way, such as Omega Centauri.[178]

text: In 2014 researchers reported that most satellite galaxies of the Milky Way actually lie in a very large disk and orbit in the same direction.[179] This came as a surprise: according to standard cosmology, the satellite galaxies should form in dark matter halos, and they should be widely distributed and moving in random directions. This discrepancy is still not fully explained.[180]

text: In January 2006, researchers reported that the heretofore unexplained warp in the disk of the Milky Way has now been mapped and found to be a ripple or vibration set up by the Large and Small Magellanic Clouds as they orbit the Milky Way, causing vibrations when they pass through its edges. Previously, these two galaxies, at around 2% of the mass of the Milky Way, were considered too small to influence the Milky Way. However, in a computer model, the movement of these two galaxies creates a dark matter wake that amplifies their influence on the larger Milky Way.[181]

text: Current measurements suggest the Andromeda Galaxy is approaching us at 100 to 140 km/s (220,000 to 310,000 mph). In 3 to 4 billion years, there may be an Andromeda–Milky Way collision, depending on the importance of unknown lateral components to the galaxies' relative motion. If they collide, the chance of individual stars colliding with each other is extremely low, but instead the two galaxies will merge to form a single elliptical galaxy or perhaps a large disk galaxy[182] over the course of about a billion years.[183]

text: Velocity

text: Although special relativity states that there is no "preferred" inertial frame of reference in space with which to compare the Milky Way, the Milky Way does have a velocity with respect to cosmological frames of reference.

text: One such frame of reference is the Hubble flow, the apparent motions of galaxy clusters due to the expansion of space. Individual galaxies, including the Milky Way, have peculiar velocities relative to the average flow. Thus, to compare the Milky Way to the Hubble flow, one must consider a volume large enough so that the expansion of the Universe dominates over local, random motions. A large enough volume means that the mean motion of galaxies within this volume is equal to the Hubble flow. Astronomers believe the Milky Way is moving at approximately 630 km/s (1,400,000 mph) with respect to this local co-moving frame of reference.[184] The Milky Way is moving in the general direction of the Great Attractor and other galaxy clusters, including the Shapley supercluster, behind it.[185] The Local Group (a cluster of gravitationally bound galaxies containing, among others, the Milky Way and the Andromeda Galaxy) is part of a supercluster called the Local Supercluster, centered near the Virgo Cluster: although they are moving away from each other at 967 km/s (2,160,000 mph) as part of the Hubble flow, this velocity is less than would be expected given the 16.8 million pc distance due to the gravitational attraction between the Local Group and the Virgo Cluster.[186]

text: Another reference frame is provided by the cosmic microwave background (CMB). The Milky Way is moving at 552 ± 6 km/s (1,235,000 ± 13,000 mph)[187] with respect to the photons of the CMB, toward 10.5 right ascension, −24° declination (J2000 epoch, near the center of Hydra). This motion is observed by satellites such as the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP) as a dipole contribution to the CMB, as photons in equilibrium in the CMB frame get blue-shifted in the direction of the motion and red-shifted in the opposite direction.[187]

text: Etymology and mythology

text: In Babylonia, the Milky Way was said to be the tail of Tiamat, set in the sky by Marduk after he had slain the salt water goddess. It is believed this account, from the Enuma Elish had Marduk replace an earlier Sumerian story when Enlil of Nippur had slain the goddess.

text: Llys Dôn (literally "The Court of Dôn") is the traditional Welsh name for the constellation Cassiopeia. At least three of Dôn's children also have astronomical associations: Caer Gwydion ("The fortress of Gwydion") is the traditional Welsh name for the Milky Way, and Caer Arianrhod ("The Fortress of Arianrhod") being the constellation of Corona Borealis.

text: In western culture the name "Milky Way" is derived from its appearance as a dim un-resolved "milky" glowing band arching across the night sky. The term is a translation of the Classical Latin via lactea, in turn derived from the Hellenistic Greek γαλαξίας, short for γαλαξίας κύκλος (galaxías kýklos, "milky circle"). The Ancient Greek γαλαξίας (galaxias) – from root γαλακτ-, γάλα ("milk") + -ίας (forming adjectives) – is also the root of "galaxy", the name for our, and later all such, collections of stars.[25][188][189][190] In Greek mythology it was supposedly made from the forceful suckling of Heracles, when Hera acted as a wetnurse for the hero.

text: The Milky Way, or "milk circle", was just one of 11 "circles" the Greeks identified in the sky, others being the zodiac, the meridian, the horizon, the equator, the tropics of Cancer and Capricorn, Arctic and Antarctic circles, and two colure circles passing through both poles.[191]

text: Astronomical history

text: In Meteorologica (DK 59 A80), Aristotle (384–322 BC) wrote that the Greek philosophers Anaxagoras (c. 500–428 BC) and Democritus (460–370 BC) proposed that the Milky Way might consist of distant stars.[192] However, Aristotle himself believed the Milky Way to be caused by "the ignition of the fiery exhalation of some stars which were large, numerous and close together"[193] and that the "ignition takes place in the upper part of the atmosphere, in the region of the world which is continuous with the heavenly motions."[194][195] The Neoplatonist philosopher Olympiodorus the Younger (c. 495–570 A.D.) criticized this view, arguing that if the Milky Way were sublunary, it should appear different at different times and places on Earth, and that it should have parallax, which it does not. In his view, the Milky Way is celestial. This idea would be influential later in the Islamic world.[196]

text: The Persian astronomer Abū Rayhān al-Bīrūnī (973–1048) proposed that the Milky Way is "a collection of countless fragments of the nature of nebulous stars".[197] The Andalusian astronomer Avempace (d 1138) proposed the Milky Way to be made up of many stars but appears to be a continuous image due to the effect of refraction in Earth's atmosphere, citing his observation of a conjunction of Jupiter and Mars in 1106 or 1107 as evidence.[195] Ibn Qayyim Al-Jawziyya (1292–1350) proposed that the Milky Way is "a myriad of tiny stars packed together in the sphere of the fixed stars" and that these stars are larger than planets.[198]

text: According to Jamil Ragep, the Persian astronomer Naṣīr al-Dīn al-Ṭūsī (1201–1274) in his Tadhkira writes: "The Milky Way, i.e. the Galaxy, is made up of a very large number of small, tightly clustered stars, which, on account of their concentration and smallness, seem to be cloudy patches. Because of this, it was likened to milk in color."[199]

text: Actual proof of the Milky Way consisting of many stars came in 1610 when Galileo Galilei used a telescope to study the Milky Way and discovered that it is composed of a huge number of faint stars.[200][201] In a treatise in 1755, Immanuel Kant, drawing on earlier work by Thomas Wright,[202] speculated (correctly) that the Milky Way might be a rotating body of a huge number of stars, held together by gravitational forces akin to the Solar System but on much larger scales.[203] The resulting disk of stars would be seen as a band on the sky from our perspective inside the disk. Kant also conjectured that some of the nebulae visible in the night sky might be separate "galaxies" themselves, similar to our own. Kant referred to both the Milky Way and the "extragalactic nebulae" as "island universes", a term still current up to the 1930s.[204][205][206]

text: The first attempt to describe the shape of the Milky Way and the position of the Sun within it was carried out by William Herschel in 1785 by carefully counting the number of stars in different regions of the visible sky. He produced a diagram of the shape of the Milky Way with the Solar System close to the center.[207]

text: In 1845, Lord Rosse constructed a new telescope and was able to distinguish between elliptical and spiral-shaped nebulae. He also managed to make out individual point sources in some of these nebulae, lending credence to Kant's earlier conjecture.[208]

text: In 1917, Heber Curtis had observed the nova S Andromedae within the Great Andromeda Nebula (Messier object 31). Searching the photographic record, he found 11 more novae. Curtis noticed that these novae were, on average, 10 magnitudes fainter than those that occurred within the Milky Way. As a result, he was able to come up with a distance estimate of 150,000 parsecs. He became a proponent of the "island universes" hypothesis, which held that the spiral nebulae were actually independent galaxies.[209] In 1920 the Great Debate took place between Harlow Shapley and Heber Curtis, concerning the nature of the Milky Way, spiral nebulae, and the dimensions of the Universe. To support his claim that the Great Andromeda Nebula is an external galaxy, Curtis noted the appearance of dark lanes resembling the dust clouds in the Milky Way, as well as the significant Doppler shift.[210]

text: The controversy was conclusively settled by Edwin Hubble in the early 1920s using the Mount Wilson observatory 2.5 m (100 in) Hooker telescope. With the light-gathering power of this new telescope, he was able to produce astronomical photographs that resolved the outer parts of some spiral nebulae as collections of individual stars. He was also able to identify some Cepheid variables that he could use as a benchmark to estimate the distance to the nebulae. He found that the Andromeda Nebula is 275,000 parsecs from the Sun, far too distant to be part of the Milky Way.[211][212]

text: Mapping

text: The ESA spacecraft Gaia provides distance estimates by determining the parallax of a billion stars and is mapping the Milky Way with four planned releases of maps in 2022.[213][214]


document_title: Children's hospital

question_text: when was the first children's hospital built

question_tokens: when was the first children 's hospital built

text: Children's hospital

text: History[edit]

text: Early Voluntary Care[edit]

text: Prior to the 19th century hospital reforms, the well-being of the child was thought to be in the hands of the mother; therefore, there was little discussion of children's medicine, and as a result next to no widespread formal institutions which focused on healing children. There were however centres which focused on helping abandoned children and offering care in hopes that these children might survive into adulthood. Some examples include orphanages, dispensaries, and foundling hospitals. Florence's Hospital of the Innocent (Ospedale degli Innocenti) was originally a charity based orphanage which opened in 1445; its aim was to nurse sick and abandoned infants back to health. A later example and better established institution whose goal it was to help rehabilitate infants was the Foundling Hospital founded by Thomas Coram in 1741. Foundling hospitals were set up to receive abandoned infants, nurse them back to health, teach them a trade or skill, and integrate them back into society. Coram's foundling hospital was revolutionary because it was one of the United Kingdoms first children charities.[4] Moreover, it was largely made successful by the powerful people who donated money to the hospital.[5] Coram's hospital would eventually be faced with the fact that the number of infants needing care outweighed their hospitals capacity. In order to accommodate the number of children in need, there were attempts to set up similar hospitals throughout the UK; they ultimately were unsuccessful due to the lack of funding.[5] Simultaneously, dispensaries which were also funded by donations were being opened in order to provide medicine and medical attention to those who could not afford private care. Dispensaries and foundling hospitals were the earliest forms of what would later become children's hospitals. The establishing of the Foundling Hospital by Thomas Coram was a direct response to the high infant mortality rate in London, England. Although foundling hospitals acknowledged the high infant mortality rate, infant mortality would not be addressed in a wide spread way until the early 19th century when children's hospitals would begin to open in Vienna, Moscow, Prague, Berlin, and various other major cities throughout Europe.[6]

text: 19th-century models[edit]

text: In America, by the mid-19th century middle-class women and physicians became increasingly concerned about the well-being of children in poor living conditions. Although infant mortality had begun to decline, it still remained a prominent issue. Social reformers blamed the emergence of the industrial society and poor parents for not properly caring for their children.[7] In response, reformers and physicians founded children's hospitals across the country. Early children's hospitals were set up in converted houses not only to help the children transition from leaving their home to being in a hospital, but also because it was often the only space available.[7] Early children's hospitals focused more on short-term care and treating mild illnesses rather than long-term intensive care. Treating serious diseases and illnesses in early children's hospitals could result in the disease spreading throughout the hospital which would drain their already limited resources. A serious disease outbreak in a children's hospital would result in more deaths than lives saved and would therefore reinforce the previous notion that people often died while in the hospital.[7]

text: Like those found in the United States, children's hospitals in the United Kingdom in the 19th century often resembled middle-class homes. British children's hospitals introduced rules to which patients and their families were expected to adhere; these rules carefully lined out middle-class values and expectations.[6] British children's hospitals, like their American and Canadian counterparts, relied heavily on donations from the rich. Donations came in the form of money, food, toys, and clothes for the children. The United Kingdom's children's hospitals were soon faced with the reality that their small and vulnerable patient would soon outnumber their resources.[6] In order to maintain the cost of running these new hospitals throughout the United Kingdom, the upper classes needed to market their hospitals as centres for reform. In order to brand themselves as reformers, they had to contrast themselves against the parents; this meant they had to portray the poor parents as incompetent.[6] Despite their mission to save children, hospitals in Britain and Glasgow rarely admitted children under the age of two; such children were deemed costly and needed constant attention.[6] Similar to the American hospitals, those located in Europe were also hesitant to admit children who required long-term care in fear that those lives would be lost or that long-term care would block beds for those in immediate need.[6] The intentions of the hospitals built in Europe were to provide care for those who could not afford care. Care was primarily provided to those who met the age requirements and were willing to adhere to the hospital's rules. Since early children's hospitals relied on donations, they were often underfunded, overcrowded, and lacking medical resources.

text: The first formally recognized paediatrics hospital was the Hôpital des Enfants Malades in Paris, France, which opened in 1802. The United Kingdom was slow to follow and established The Great Ormond Street Hospital in London, England, in 1852, which marked the opening of the first British children's hospital.[8] The United States would soon follow and established The Children's Hospital of Philadelphia in Pennsylvania in 1855.[9] Canada established their first children's hospital in 1875; The Hospital for Sick Children in Toronto, Ontario, along with the latter all remain open today.[10] By the end of the 19th century, and the during the first two decades of the 20th century, the number of children's hospitals tripled in both Canada and the United States.[7] The first children's hospital in Scotland opened in 1860 in Edinburgh.[11]

text: Professionalization of Children's Hospitals[edit]

text: In the 19th century, there was a societal shift in how children were viewed. This shift took away some of the parents' control and placed it in the hands of medical professionals.[12] By the early 20th century, a child's health became increasingly tied to physicians and hospitals. Unlike the professionalization of nursing, the medical field professionalized at a greater speed.[13] This was a result of licensing acts, the formation of medical associations, and new fields of medicine being introduced across countries.[13] These new areas of medicine offered physicians the chance to build their careers by "overseeing the medical needs of private patients, caring for and trying new therapies on the sick poor, and teaching medical students."[13] In order to raise their status further, physicians began organizing children's hospitals; by doing so, it also brought attention and importance to their speciality in the modern health care system.[7] This idea brought about the creation of children's hospitals in Philadelphia, Boston, Washington, D.C, and San Francisco – all which emphasized children as their focus.[7] Along with specialized physicians, the 20th century brought the removal of voluntary or religiously associated female care and replaced it with professionally trained nurses.[14] In addition to separate institutions for children and a professional staff, both medical and technological advancement helped solidify children's hospitals as centres of physical healing. The discovery of vaccines, anaesthetics, and surgical improvements made children's hospitals more reliable and more effective in the treatment of childhood disease and illness.

text: Utilization[edit]

text: Using hospital discharge data from 2003-2011, the Agency for Healthcare Research and Quality (AHRQ) studied trends in aggregate hospital costs, average hospital costs, and hospital utilization. The Agency found that for children aged 0–17, aggregate costs rose rapidly for the surgical hospitalizations and decreased for injury hospitalizations. Further, average hospital costs, or cost per discharge, increased at least 2% for all hospitalizations and were expected to grow by at least 4% through 2013. The exception to this was mental health hospitalizations, which saw a lower percentage increase of 1.2%, and was projected to increase only 0.9% through 2013. Despite the rising aggregate costs and costs per discharge, hospitalizations (except for mental health hospitalizations) for children aged 0–17 decreased over the same time, and were projected to continue decreasing.[15]

text: In 2006-2011, the rate of ED use in the United States was highest for patients aged under one year, but lowest for patients aged 1–17 years. The rate of ED use for patients aged under one year declined over the same time period; this was the only age group to see a decline.[16]

text: Between 2008 and 2012, growth in mean hospital costs per stay in the United States was highest for patients aged 17 and younger.[17] In 2012 there were nearly 5.9 million hospital stays for children in the United States, of which 3.9 million were neonatal stays and 104,700 were maternal stays for pregnant teens.[18]

text: Ranking[edit]

text: Every year US News & World Report ranks the top children's hospitals and pediatric specialties in the United States. For the year 2010-2011, eight hospitals ranked in all 10 pediatric specialties. The ranking system used by US News & World Report depends on a variety of factors. In past years (2007 was the 18th year of Pediatric Ranking), ranking of hospitals has been done solely on the basis of reputation, gauged by random sampling and surveying of pediatricians and pediatric specialists throughout the country. The ranking system used is currently under review.[19]


document_title: List of Los Angeles Angels no-hitters

question_text: when was the last time the angels were no hit

text: List of Los Angeles Angels no-hitters

text: List of no-hitters in Angels history[edit]

text:
¶
Indicates a perfect game

 £
Pitcher was left-handed

 *
Member of the National Baseball Hall of Fame and Museum

text:
#
Date
Pitcher
Final score
Base-
runners
Opponent
Catcher
Plate umpire
Manager
Notes
Ref

1
000000001962-05-05-0000May 5, 1962
Belinsky, BoBo Belinsky
7000200000000000000♠2–0
7
Baltimore Orioles
Rodgers, BuckBuck Rodgers
Schwarts, HarryHarry Schwarts
Rigney, BillBill Rigney

First no-hitter in franchise history
First Angels no-hitter at home
First left-handed pitcher to throw a no-hitter in franchise history

[7]

2
000000001970-07-03-0000July 3, 1970
Wright, ClydeClyde Wright£
7000400000000000000♠4–0
3
Oakland Athletics
Azcue, JoeJoe Azcue
Springstead, MartyMarty Springstead
Phillips, LeftyLefty Phillips

In a pre-game ceremony, Wright had been inducted into the NAIA Hall of Fame

[8]

3
000000001973-05-15-0000May 15, 1973
Ryan, NolanNolan Ryan* (1)
7000300000000000000♠3–0
3
@ Kansas City Royals
Torborg, JeffJeff Torborg
Evans, JimJim Evans
Winkles, BobbyBobby Winkles (1)

First Angels no-hitter on the road
First right-handed pitcher to throw a no-hitter in franchise history
1st of 7 no-hitters for Ryan

[9]

4
000000001973-07-15-0000July 15, 1973
Ryan, NolanNolan Ryan* (2)
7000600000000000000♠6–0
4
@ Detroit Tigers
Kusnyer, ArtArt Kusnyer
Luciano, RonRon Luciano
Winkles, BobbyBobby Winkles (2)

2nd of 7 no-hitters for Ryan
Shortest interval between no-hitters in franchise history
Pitched 7 innings of no-hit ball in next start, closest to tying Vander Meer's back-to-back no-hitters since Ewell Blackwell in 1947

[10]

5
000000001974-09-28-0000September 28, 1974
Ryan, NolanNolan Ryan* (3)
7000400000000000000♠4–0
8
Minnesota Twins
Egan, TomTom Egan
Frantz, ArtArt Frantz
Williams, DickDick Williams (1)

3rd of 7 no-hitters for Ryan
Most baserunners allowed in an Angels no-hitter

[11]

6
000000001975-06-01-0000June 1, 1975
Ryan, NolanNolan Ryan* (4)
7000100000000000000♠1–0
5
Baltimore Orioles
Rodriguez, EllieEllie Rodriguez
Morgenweck, HankHank Morgenweck
Williams, DickDick Williams (2)

4th of 7 no-hitters for Ryan
Smallest margin of victory in an Angels no-hitter (tie)

[12]

7
000000001984-09-30-0000September 30, 1984
Witt, MikeMike Witt¶
7000100000000000000♠1–0
0
@ Texas Rangers
Boone, BobBob Boone
Froemming, BruceBruce Froemming
McNamara, JohnJohn McNamara

Final game of season
First and only perfect game in Angels history and 11th in MLB history
Smallest margin of victory in an Angels no-hitter (tie)
Latest calendar date of an Angels no-hitter

[13]

8
000000001990-04-11-0000April 11, 1990
Langston, MarkMark Langston£ (7 IP)
Mike Witt (2 IP)
7000100000000000000♠1–0
5
Seattle Mariners
Parrish, LanceLance Parrish
Voltaggio, VicVic Voltaggio
Rader, DougDoug Rader

Smallest margin of victory in an Angels no-hitter (tie)
Game 3 of season
Earliest calendar date of an Angels no-hitter

[14]

9
000000002011-07-27-0000July 27, 2011
Santana, ErvinErvin Santana
7000300000000000000♠3–1
2
@ Cleveland Indians
Wilson, BobbyBobby Wilson
Barrett, TedTed Barrett
Scioscia, MikeMike Scioscia (1)

First Angels no-hitter while allowing a run
Santana's first career win against Cleveland
First no-hitter at Progressive Field (formerly Jacobs Field)

[15]

10
000000002012-05-02-0000May 2, 2012
Weaver, JeredJered Weaver
7000900000000000000♠9–0
2
Minnesota Twins
Iannetta, ChrisChris Iannetta
Carlson, MarkMark Carlson
Scioscia, MikeMike Scioscia (2)

Most recent no-hitter in franchise history
Largest margin of victory in an Angels no-hitter

[16]