astronomy

WN B1127.5+4927

WN B1127.5+4927 is a astronomy topic covered in the lgStudy science library. This page brings together a partial reference excerpt, illustrations, worked examples, real-world applications and a short study plan, so you can understand WN B1127.5+4927 rather than just read about it. In short: WN B1127.5+4927 also known as RGZ J113018.3+491116 and NYU-VAGC 0795797, is a radio galaxy located in the constellation of Ursa Major. The redshift of the galaxy is (z) 0.260 and it was first discovered as a background astronomical radio source by astronomers in January 1989.

Key takeaways

WN B1127.5+4927 belongs to astronomy; place it in that map before memorising details.
Learn the definition first, then one example that makes the definition concrete.
Connect WN B1127.5+4927 to a quantity you can measure, compute or draw — that is where exam questions come from.
Reproduce the core statement of WN B1127.5+4927 from memory before moving on to harder problems.

Reference excerpt

WN B1127.5+4927 also known as RGZ J113018.3+491116 and NYU-VAGC 0795797, is a radio galaxy located in the constellation of Ursa Major. The redshift of the galaxy is (z) 0.260 and it was first discovered as a background astronomical radio source by astronomers in January 1989.

Description WN B1127.5+4927 is a red luminous galaxy residing as the brightest cluster galaxy of the WHL J113018.3+491116 galaxy cluster with 29 confirmed galaxy member candidates. The R-band magnitude of the galaxy has been estimated to be 17.46 magnitude while the absolute magnitude is -23.20. Its stellar velocity dispersion is calculated to be 284 kilometers per seconds and has an effective radius of 13.8 kiloparsecs. The total physical size of the galaxy is 222 kiloparsecs. The R-band luminosity is 6.90 × 1010 Lʘ while the Z-band luminosity is 8.47 × 1010 Lʘ. The central nucleus is found to be active and is categorized as a bend Fanaroff-Riley Class Type II radio galaxy hosting a FRII-like radio source. The total flux density measured by NRAO VLA Sky Survey (NVSS) has been estimated to be 15.90 mJy at 1.4 GHz frequencies. The angular size of the source is 39 arcseconds whereas the linear size is 157.2 kiloparsecs. The total radio luminosity at 1.4 GHz is 25.04 W Hz-1. A study published in 2012, has found a pair of resolved radio lobes. The projected length of the first lobe is found to be 81.1 kiloparsecs while the second lobe has a projected length of 118.1 kiloparsecs. The angular separation of the lobes are estimated to be 12.7 and 18.4 arcseconds respectively. The galaxy also contains a presence of a double radio source with an unresolved radio core. The eastern and western lobes have linear sizes of 100 × 52 and 80 × 72 kiloparsecs respectively in total. Evidence also found the source is bend with a measured bending angle of 0.0° while the excess bending angle is -7.3°.

References

External links WN B1127.5+4927 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images

Illustrations

Worked examples

Example 1 — a first encounter with WN B1127.5+4927

Start with the simplest possible case. Write down what WN B1127.5+4927 claims or describes in one sentence, then invent the smallest concrete situation in which that sentence is true. In astronomy, the smallest case is usually a single object, a single equation or a single measurement. Check that every symbol or term in your sentence has a meaning in that case.

Example 2 — changing one variable

Take the situation from Example 1 and change exactly one quantity: double it, halve it, or set it to zero. Predict what should happen to WN B1127.5+4927 before you calculate. Comparing your prediction with the result is the fastest way to find out whether you understand the idea or only the words.

Example 3 — an exam-style question

Typical questions about WN B1127.5+4927 ask you to (a) state it precisely, (b) apply it to given data, and (c) explain a limitation. Practise writing all three answers in under five minutes; the third part is what separates a full-mark answer from an average one.

Applications of WN B1127.5+4927

In research: WN B1127.5+4927 appears in astronomy research whenever the underlying quantities have to be modelled precisely. Papers usually cite it as a starting assumption and then explore where it breaks down.
In technology and industry: Engineering practice reuses WN B1127.5+4927 in design rules, simulations and safety margins. Knowing the idea lets you read a specification sheet and understand why the numbers look the way they do.
In the classroom: WN B1127.5+4927 is common in secondary-school and first-year university syllabi. It links to neighbouring topics Active galaxies, Astronomical objects discovered in 1989, LEDA objects, so understanding it makes those chapters shorter.
In everyday life: Look for WN B1127.5+4927 outside the textbook — in sport, cooking, traffic, electronics or the sky above you. An example you found yourself is remembered far longer than one you were given.

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How to study WN B1127.5+4927 in 20 minutes

Read the reference excerpt below once, without taking notes.
Close the page and write down what WN B1127.5+4927 means in your own words.
Compare your version with the excerpt and mark what you missed.
Work through the three examples above with pen and paper.
Explain WN B1127.5+4927 out loud to somebody else — or to Teacher Smith in the lgStudy chat.

Frequently asked questions

What is WN B1127.5+4927 in simple terms?

Why does WN B1127.5+4927 matter?

Because it connects several astronomy ideas at once: it gives you a definition you can apply, a quantity you can calculate, and a way to check whether a result is plausible.

How should I study WN B1127.5+4927?

Read the excerpt, restate it from memory, then work through the examples and applications listed on this page. The five-step study plan above takes about twenty minutes.

What does this page cover?

It gives you a compact reference excerpt plus original lgStudy explanations, examples, applications and study material on WN B1127.5+4927.