An Etymological Dictionary of Astronomy and Astrophysics

Last; furthest or farthest; conclusive in a process or series; the highest or most significant.

Etymology (EN): L.L. ultimatus, p.p. of ultimare “to be final, come to an end,” from L. ultimus “last, final, farthest, extreme,” superlative of *ulter “beyond.”

Etymology (PE): Ultom, from ul “up, upward,” ulêh “upward, above,” → ultra-, + -tom supelative suffix, → extreme.
Farjâmin “belonging to the end; concluding,” from farjâm “end; conclusion,” from Mid.Pers. farzâm “end; conclusion,” farzâftan “to finish, to be perfect;” from Proto-Iranian *fra-gam- “to send; to finish” (cf. O.Pers. prāgama- “to go forth”), from *gam- “to go; to come;” cf. Av. gam- “to come; to go,” jamaiti “goes;” O.Pers. gam- “to come; to go;” Mod./Mid.Pers. gâm “step, pace,” âmadan “to come;” cf. Skt. gamati “goes;” Gk. bainein “to go, walk, step;” L. venire “to come;” Tocharian A käm- “to come;” O.H.G. queman “to come;” E. come; PIE root *gwem- “to go, come.”

Last; furthest or farthest; conclusive in a process or series; the highest or most significant.

Etymology (EN): L.L. ultimatus, p.p. of ultimare “to be final, come to an end,” from L. ultimus “last, final, farthest, extreme,” superlative of *ulter “beyond.”

Etymology (PE): Ultom, from ul “up, upward,” ulêh “upward, above,” → ultra-, + -tom supelative suffix, → extreme.
Farjâmin “belonging to the end; concluding,” from farjâm “end; conclusion,” from Mid.Pers. farzâm “end; conclusion,” farzâftan “to finish, to be perfect;” from Proto-Iranian *fra-gam- “to send; to finish” (cf. O.Pers. prāgama- “to go forth”), from *gam- “to go; to come;” cf. Av. gam- “to come; to go,” jamaiti “goes;” O.Pers. gam- “to come; to go;” Mod./Mid.Pers. gâm “step, pace,” âmadan “to come;” cf. Skt. gamati “goes;” Gk. bainein “to go, walk, step;” L. venire “to come;” Tocharian A käm- “to come;” O.H.G. queman “to come;” E. come; PIE root *gwem- “to go, come.”

The future evolution of the → Universe which is a subject of study in → cosmology. The ultimate fate of the Universe can be explored using → general relativity.
And since there is more than one possible solution to the equations of general relativity, there is more than one possible ultimate fate of the Universe. Moreover, the fate will depend on three factors: the Universe’s overall shape or → geometry, its → dark energy content, and the → equation of state parameter. See also: → oscillating Universe, → Big Rip, → Big Crunch, → Big Freeze, → heat death.

See also: → ultimate; → Universe.

The future evolution of the → Universe which is a subject of study in → cosmology. The ultimate fate of the Universe can be explored using → general relativity.
And since there is more than one possible solution to the equations of general relativity, there is more than one possible ultimate fate of the Universe. Moreover, the fate will depend on three factors: the Universe’s overall shape or → geometry, its → dark energy content, and the → equation of state parameter. See also: → oscillating Universe, → Big Rip, → Big Crunch, → Big Freeze, → heat death.

See also: → ultimate; → Universe.

A prefix occurring originally in loanwords from L., with the basic meaning “on the far side of, beyond, extremely.”

Etymology (EN): From L. ultra- from ultra (adverb and preposition) “beyond, on the further side,” from ulter, from uls “beyond;” + -ter suffix of comparative adj.; PIE base *al- “besides, other, beyond.”

Etymology (PE): Ultar-, from Mid.Pers. ul “up, upward,” ulêh “upward, above” (Av. ərəδuua- “upright, risen; cf. Skt. ūrdhvá- “high, above, elevated; Gr. orthos “set upright, straight;”
L. arduus “high, steep;” → ortho-)

• -tar suffix forming comparative adjectives (Mid.Pers. -tar; Av. -tara- (masculine); PIE base *-tero).

A prefix occurring originally in loanwords from L., with the basic meaning “on the far side of, beyond, extremely.”

Etymology (EN): From L. ultra- from ultra (adverb and preposition) “beyond, on the further side,” from ulter, from uls “beyond;” + -ter suffix of comparative adj.; PIE base *al- “besides, other, beyond.”

Etymology (PE): Ultar-, from Mid.Pers. ul “up, upward,” ulêh “upward, above” (Av. ərəδuua- “upright, risen; cf. Skt. ūrdhvá- “high, above, elevated; Gr. orthos “set upright, straight;”
L. arduus “high, steep;” → ortho-)

• -tar suffix forming comparative adjectives (Mid.Pers. -tar; Av. -tara- (masculine); PIE base *-tero).

A galaxy of low stellar density, defined to have low central → surface brightness (> 24 mag arcsec^-2) and an → effective radius (R_e) of over 1.5 kpc. The question of whether UDGs represent a separate class of galaxies is still under debate. Currently, known UDGs that have been discovered in clusters, in groups, and in the field can have R_e as large as 5 kpc which is comparable to that of giant Milky Way like galaxies. This fact has been used to suggest that UDGs are “failed” giants. As R_e captures (at most) the central parts of giant galaxies, whether this radius can be used to fairly compare the sizes of UDGs to the more massive galaxies is questionable (see, e.g., Chamba et al., 2020, A&A 633, L3).

See also: Term proposed by van Dokkum et al. (2015), arXiv: 1410.8141v2; → ultra-; → diffuse; → galaxy.

A galaxy of low stellar density, defined to have low central → surface brightness (> 24 mag arcsec^-2) and an → effective radius (R_e) of over 1.5 kpc. The question of whether UDGs represent a separate class of galaxies is still under debate. Currently, known UDGs that have been discovered in clusters, in groups, and in the field can have R_e as large as 5 kpc which is comparable to that of giant Milky Way like galaxies. This fact has been used to suggest that UDGs are “failed” giants. As R_e captures (at most) the central parts of giant galaxies, whether this radius can be used to fairly compare the sizes of UDGs to the more massive galaxies is questionable (see, e.g., Chamba et al., 2020, A&A 633, L3).

See also: Term proposed by van Dokkum et al. (2015), arXiv: 1410.8141v2; → ultra-; → diffuse; → galaxy.

A particle belonging to the most energetic population of → cosmic rays with an energy above ~ 10²⁰ → electron-volts. The UHECRs constitute a real challenge for theoretical models, because their acceleration requires extreme conditions hardly fulfilled by known astrophysical objects. See also → UHECR puzzle, → Greisen-Zatsepin-Kuzmin cutoff.

See also: → ultra- + → high-energy cosmic ray.

A particle belonging to the most energetic population of → cosmic rays with an energy above ~ 10²⁰ → electron-volts. The UHECRs constitute a real challenge for theoretical models, because their acceleration requires extreme conditions hardly fulfilled by known astrophysical objects. See also → UHECR puzzle, → Greisen-Zatsepin-Kuzmin cutoff.

See also: → ultra- + → high-energy cosmic ray.

A neutrino particle accelerated to energies above 10¹⁸ → electron-volts. They are produced by the interaction of → ultra-high-energy cosmic ray (UHECR)s with the → cosmic microwave background radiation. Also called → cosmogenic neutrinos. See also → Greisen-Zatsepin-Kuzmin limit.

See also: → ultra-; → high; → energy; → neutrino.

A neutrino particle accelerated to energies above 10¹⁸ → electron-volts. They are produced by the interaction of → ultra-high-energy cosmic ray (UHECR)s with the → cosmic microwave background radiation. Also called → cosmogenic neutrinos. See also → Greisen-Zatsepin-Kuzmin limit.

See also: → ultra-; → high; → energy; → neutrino.

Extremely compact with respect to a comparison value. → ultracompact H II region, → ultracompact dwarf galaxy.

See also: → ultra-; → compact.

Extremely compact with respect to a comparison value. → ultracompact H II region, → ultracompact dwarf galaxy.

See also: → ultra-; → compact.

A type of very bright compact → stellar system (-14 ≤ M_V≥ -12) that is intermediate between → globular clusters (GCs) and → compact elliptical galaxies (cEs). With masses of M > 2 × 10⁶ Msun and radii > 10 → parsecs (pc), UCDs are among the densest stellar systems in the Universe. Nevertheless, the nature and origin of these objects is still widely debated. Early interpretations suggested that UCDs could be the most massive GCs or possibly the → tidally stripped remnants of → dwarf galaxies. However, there is evidence that both formation mechanisms could contribute to the UCD population. → Supermassive black holes (SMBHs) have been confirmed in most UCDs with masses M > 10⁷ Msun.

The most massive UCD discovered to date, M59-UCD3 (M_* ~ 2 × 10⁸ Msun, radius ~ 25 pc), hosts a SMBH (Ahn et al., 2018, arxiv/1804.02399, and references therein).

See also: → ultracompact; → dwarf; → galaxy.

A type of very bright compact → stellar system (-14 ≤ M_V≥ -12) that is intermediate between → globular clusters (GCs) and → compact elliptical galaxies (cEs). With masses of M > 2 × 10⁶ Msun and radii > 10 → parsecs (pc), UCDs are among the densest stellar systems in the Universe. Nevertheless, the nature and origin of these objects is still widely debated. Early interpretations suggested that UCDs could be the most massive GCs or possibly the → tidally stripped remnants of → dwarf galaxies. However, there is evidence that both formation mechanisms could contribute to the UCD population. → Supermassive black holes (SMBHs) have been confirmed in most UCDs with masses M > 10⁷ Msun.

The most massive UCD discovered to date, M59-UCD3 (M_* ~ 2 × 10⁸ Msun, radius ~ 25 pc), hosts a SMBH (Ahn et al., 2018, arxiv/1804.02399, and references therein).

See also: → ultracompact; → dwarf; → galaxy.

A very young → H II region fully embedded in its natal molecular cloud.
Ultracompact H II regions are distinguished from classical H II regions by their small sizes (diameter ≥ 0.1 pc), high densities (Ne ≥ 10⁵ cm^-3), and high emission measures (EM ≥ 10⁷ pc cm^-6). Their typical ionized gas content is about 10^-2  → solar masses, in contrast to classical H II regions with a mass of about 10⁵ solar masses. Due to very important extinction, ultracompact H II regions are not accessible to visible wavelengths.

See also: → ultra-; → compact; → H II region.

A very young → H II region fully embedded in its natal molecular cloud.
Ultracompact H II regions are distinguished from classical H II regions by their small sizes (diameter ≥ 0.1 pc), high densities (Ne ≥ 10⁵ cm^-3), and high emission measures (EM ≥ 10⁷ pc cm^-6). Their typical ionized gas content is about 10^-2  → solar masses, in contrast to classical H II regions with a mass of about 10⁵ solar masses. Due to very important extinction, ultracompact H II regions are not accessible to visible wavelengths.

See also: → ultra-; → compact; → H II region.

A star-like objects with an → effective temperature of less than 2,700 K. Ultracool dwarfs constitute a heterogeneous group including stars of extremely low mass as well as → brown dwarfs, and represent about 15% of the population of astronomical objects near the Sun.

See also: → ultra-; → cool; → dwarf.

A star-like objects with an → effective temperature of less than 2,700 K. Ultracool dwarfs constitute a heterogeneous group including stars of extremely low mass as well as → brown dwarfs, and represent about 15% of the population of astronomical objects near the Sun.

See also: → ultra-; → cool; → dwarf.

The quality of an object whose → luminosity exceeds a certain value.

See also: → ultra-; → luminous.

The quality of an object whose → luminosity exceeds a certain value.

See also: → ultra-; → luminous.

A galaxy that emits more than 90% of its energy in the infrared (8-1000 µm) and
whose infrared luminosity exceeds 10¹² solar luminosities. → luminous infrared galaxy (LIRG). Quasars can also have such high or even higher bolometric luminosities. However LIRGs and ULIRGs emit the bulk of their energy in the infrared. Most of ULIRGs are found in merging and interacting galaxy systems. It is thought that their luminosity results from galactic collisions, which increase the rate of star formation.

See also: → ultraluminous; → infrared; → galaxy.

A galaxy that emits more than 90% of its energy in the infrared (8-1000 µm) and
whose infrared luminosity exceeds 10¹² solar luminosities. → luminous infrared galaxy (LIRG). Quasars can also have such high or even higher bolometric luminosities. However LIRGs and ULIRGs emit the bulk of their energy in the infrared. Most of ULIRGs are found in merging and interacting galaxy systems. It is thought that their luminosity results from galactic collisions, which increase the rate of star formation.

See also: → ultraluminous; → infrared; → galaxy.

An X-ray source that is not in the nucleus of a galaxy, and is more luminous than 10³⁹ ergs s^-1, brighter than the → Eddington luminosity of a 10 → solar mass → black hole. In general, there is about one ULX per galaxy in galaxies which host ULXs. The Milky Way contains no such objects. ULXs are thought to be powered by → accretion onto a → compact object. Possible explanations include accretion onto → neutron stars
with strong → magnetic fields, onto → stellar black holes (of up to 20 → solar masses) at or in excess of the classical Eddington limit, or onto → intermediate-mass black holes (10³-10⁵ solar masses). NGC 1313X-1, NGC 5408X-1, and NGC 6946X-1 are three ULXs with X-ray luminosities up to ~ 10⁴⁰ erg s^-1 (Ciro Pinto et al., 2016, Nature 533, N) 7601).

See also: → ultraluminous; → X-ray source.

An X-ray source that is not in the nucleus of a galaxy, and is more luminous than 10³⁹ ergs s^-1, brighter than the → Eddington luminosity of a 10 → solar mass → black hole. In general, there is about one ULX per galaxy in galaxies which host ULXs. The Milky Way contains no such objects. ULXs are thought to be powered by → accretion onto a → compact object. Possible explanations include accretion onto → neutron stars
with strong → magnetic fields, onto → stellar black holes (of up to 20 → solar masses) at or in excess of the classical Eddington limit, or onto → intermediate-mass black holes (10³-10⁵ solar masses). NGC 1313X-1, NGC 5408X-1, and NGC 6946X-1 are three ULXs with X-ray luminosities up to ~ 10⁴⁰ erg s^-1 (Ciro Pinto et al., 2016, Nature 533, N) 7601).

See also: → ultraluminous; → X-ray source.

Describing a system or situation for which the → Lorentz factor, γ, is much larger than 1. See also → subrelativistic.

See also: → ultra- + → relativistic

Describing a system or situation for which the → Lorentz factor, γ, is much larger than 1. See also → subrelativistic.

See also: → ultra- + → relativistic

A gas composed of ultrarelativistic particles.

See also: → ultrarelativistic; → gas.

A gas composed of ultrarelativistic particles.

See also: → ultrarelativistic; → gas.

A → Cepheid star of → spectral type A-F with regular pulsation period of 1-3 hours and with small variations in amplitude. This group is also known as δ Scuti stars.

See also: → ultra-; → short; → period; → Cepheid.

A → Cepheid star of → spectral type A-F with regular pulsation period of 1-3 hours and with small variations in amplitude. This group is also known as δ Scuti stars.

See also: → ultra-; → short; → period; → Cepheid.

The branch of physics dealing with elastic waves of frequencies above 20 kHz to 10¹⁰ kHz propagated in solids, liquids, and gases.

See also: → ultra-; sonic from L. sonus→ sound + → -ics.

The branch of physics dealing with elastic waves of frequencies above 20 kHz to 10¹⁰ kHz propagated in solids, liquids, and gases.

See also: → ultra-; sonic from L. sonus→ sound + → -ics.

Sound with a frequency lying above the audition frequency range, usually taken to be about 20 kHz. → sound wave.

See also: → ultra- + → sound.

Sound with a frequency lying above the audition frequency range, usually taken to be about 20 kHz. → sound wave.

See also: → ultra- + → sound.

The part of the electromagnetic radiation beyond the violet end of the visible spectrum with wavelengths approximately in the range 50 Å to 4,000 Å. → extreme ultraviolet; → far ultraviolet.

See also: → ultra-; → violet.

The part of the electromagnetic radiation beyond the violet end of the visible spectrum with wavelengths approximately in the range 50 Å to 4,000 Å. → extreme ultraviolet; → far ultraviolet.

See also: → ultra-; → violet.

The study of astronomical objects in the ultraviolet portions of the electromagnetic spectrum, in the waveband 3000 Å to about 10 Å. At these wavelengths, the atmosphere prevents ultraviolet radiation from reaching the Earth surface. Therefore ground-based observatories cannot observe in the ultraviolet. Only with the advent of space-based telescopes has this area of astronomy become available for research.

See also: → ultraviolet; → astronomy.

The study of astronomical objects in the ultraviolet portions of the electromagnetic spectrum, in the waveband 3000 Å to about 10 Å. At these wavelengths, the atmosphere prevents ultraviolet radiation from reaching the Earth surface. Therefore ground-based observatories cannot observe in the ultraviolet. Only with the advent of space-based telescopes has this area of astronomy become available for research.

See also: → ultraviolet; → astronomy.

A → paradox encountered in the classical theory of → thermal radiation (→ Rayleigh-Jeans law), whereby a → blackbody should radiate an infinite amount of energy at infinitely short wavelengths, in contradiction with what is observed. The problem was solved by Max Planck in 1900, who suggested that, rather than being continuous, the energy comes in discrete parcels called → quanta. The avoidance of the ultraviolet catastrophe was one of the first great achievements of → quantum mechanics.

See also: This problem was first raised by Lord Rayleigh (1842-1919), whereas the term ultraviolet catastrophe was first used by Paul Ehrenfest (1880-1933); → ultraviolet; → catastrophe.

A → paradox encountered in the classical theory of → thermal radiation (→ Rayleigh-Jeans law), whereby a → blackbody should radiate an infinite amount of energy at infinitely short wavelengths, in contradiction with what is observed. The problem was solved by Max Planck in 1900, who suggested that, rather than being continuous, the energy comes in discrete parcels called → quanta. The avoidance of the ultraviolet catastrophe was one of the first great achievements of → quantum mechanics.

See also: This problem was first raised by Lord Rayleigh (1842-1919), whereas the term ultraviolet catastrophe was first used by Paul Ehrenfest (1880-1933); → ultraviolet; → catastrophe.

Ultraviolet emission from an object in excess of that expected for a reference.
For example, → subdwarf stars show ultraviolet excess with respect to that expected from a star with → solar metallicity
at a given → effective temperature. In this case, UV excess results from smaller → line blanketing in
→ population II stars.

See also: → ultraviolet; → excess.

Ultraviolet emission from an object in excess of that expected for a reference.
For example, → subdwarf stars show ultraviolet excess with respect to that expected from a star with → solar metallicity
at a given → effective temperature. In this case, UV excess results from smaller → line blanketing in
→ population II stars.

See also: → ultraviolet; → excess.

A star, such as O types or hot central stars of planetary nebulae, which radiates essentially in the ultraviolet part of the electromagnetic spectrum.

See also: → ultraviolet; → star.

A star, such as O types or hot central stars of planetary nebulae, which radiates essentially in the ultraviolet part of the electromagnetic spectrum.

See also: → ultraviolet; → star.