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SWEEPS-04

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SWEEPS-04
Discovery
Size comparison of SWEEPS-04 with Jupiter.
Discovered by	Sahu et al.^[1]
Discovery date	October 4, 2006
Detection method	Transit
Orbital characteristics
Semi-major axis	0.055 AU (8,200,000 km)
Orbital period (sidereal)	4.2 d
Inclination	>87
Star	SWEEPS J175853.92−291120.6
Physical characteristics
Mean radius	0.81±0.1 `R`_J
Mass	<3.8 `M`_J

SWEEPS-04 is an extrasolar planet orbiting the star SWEEPS J175853.92−291120.6 in the constellation Sagittarius approximately 27,710 light years away (based on a distance modulus of 14.1) from the Solar System, making it (along with SWEEPS-11) the most distant exoplanet(s) known.^[2] This planet was found in 2006 by the Sagittarius Window Eclipsing Extrasolar Planet Search (SWEEPS) program that uses the transit method.

The upper limit on the planet's mass is 3.8 times the mass of Jupiter. The best fit radius is 0.81 times that of Jupiter, but the uncertainty in this value is large, around 12%. It orbits at an average distance of 8,200,000 km (0.055 AU) from the parent star, taking 4.2 days to revolve around it.

HST SWEEPS-4 2006
Radial Velocities of SWEEPS-04 (UVES-VLT)
Artist's impression of a transiting Jupiter-mass exoplanet SWEEPS J175853.92-291120.6 b

References

[edit]

^ Sahu, Kailash C.; Casertano, S; Bond, HE; Valenti, J; Smith, TE; Minniti, D; Zoccali, M; Livio, M; et al. (2006). "Transiting extrasolar planetary candidates in the Galactic bulge". Nature. 443 (7111): 534–540. arXiv:astro-ph/0610098. Bibcode:2006Natur.443..534S. doi:10.1038/nature05158. PMID 17024085. S2CID 4403395. (web Preprint)
^ "HEC: Top 10 Exoplanets - Planetary Habitability Laboratory @ UPR Arecibo". phl.upr.edu. Archived from the original on 17 December 2013. Retrieved 16 July 2018.

External links

[edit]

"SWEEPS-04". Exoplanets. Archived from the original on 2009-11-25. Retrieved 2009-05-22.

Constellation of Sagittarius

Stars

Bayer	α (Rukbat) β¹ (Arkab Prior) β² (Arkab Posterior) γ¹ (W) γ² (Alnasl) δ (Kaus Media) ε (Kaus Australis) ζ (Ascella) η θ¹ θ² ι κ¹ κ² λ (Kaus Borealis) μ (Polis) ν¹ (Ainalrami) ν² ξ¹ ξ² ο π (Albaldah) ρ¹ ρ² σ (Nunki) τ υ φ χ¹ χ² χ³ ψ ω (Terebellum)
Flamsteed	1 3 4 5 6 7 9 11 12 14 15 16 17 18 21 23 24 25 26 28 29 30 31 33 43 (d) 50 51 (h¹) 52 (h²) 53 54 (e¹) 55 (e²) 56 (f) 57 59 (b) 60 (A) 61 (g) 62 (c) 63 65 63 Oph
Variable	U Y RS RY VX KW V348 V356 V630 V725 V1017 V1059 V3961 V4024 V4029 V4030 V4046 V4199 V4200 V4332 V4334 V4375 V4381 V4580 V4641 V4647 (Pistol Star) V4650 V4743 V4998 V5125 V5157 V5652 (Gumala) V5668 V5856
HR	6748 6762 6766 6836 6842 6907 6998 7029 7355 7380 7631 7652 7659 7703
HD	163296 164604 (Pincoya) 166191 169142 170657 171238 177765 180902 181342 (Belel) 181720 (Sika) 187085 190647 316285
Other	2MASS J18352154−3123385 2MASS J19281982−2640123 Bursting Pulsar CEN 16 CWISEP J1935−1546 D9 GCIRS 7 GCIRS 8* GCIRS 13E GCIRS 16SW Gomez's Hamburger G0.238−0.071 HATS-36 IRAS 17423−1755 IRAS 18162−2048 K2-2016-BLG-0005L KMT-2020-BLG-0414L LBV 1806−20 MACHO 176.18833.411 MACHO-96-BLG-5 MACHO-1997-BLG-41 MACHO-98-BLG-35 MOA-2007-BLG-192L MOA-2007-BLG-400L MOA-2009-BLG-387L MOA-2010-BLG-477L MOA-2011-BLG-262L NGC 6822-WR 12 OGLE-2003-BLG-235L OGLE-2005-BLG-169L OGLE-2011-BLG-0462 PSR J1747−2958 PSR J1748−2021B PSR J1748−2446ad PSR J1930−1852 Ross 154 S2 S55 S62 S4716 SAX J1808.4−3658 SGR J1745−2900 SGR 1806−20 SWEEPS J175853.92−291120.6 SWIFT J1745−26 SWIFT J1756.9−2508 SWIFT J1818.0−1607 W33A WASP-67 WD 0032−317 WR 101-2 WR 102 WR 102c WR 102ea WR 102ka WR 104 WR 111

Exoplanets

Star
clusters

NGC	6440 6520 6522 6528 6530 6540 6544 6553 6558 6569 6603 6624 6638 6642 6717 6723 6774
Other	1806−20 cluster 2MASS-GC02 Arches Cluster CO−0.40−0.22 Messier 18 Messier 21 Messier 22 Messier 23 Messier 25 Messier 28 Messier 54 Messier 55 Messier 69 Messier 70 Messier 75 Quintuplet Cluster Small Sagittarius Star Cloud Terzan 5 Terzan 7 Terzan 8 VVV CL001

Nebulae

NGC

Other

Galaxies

NGC	6822 6902
Other	ESO 593-8 MRC 2011−298 PKS 1830−211 PKS 2000−330 PKS 2004−447 Sagittarius Dwarf Irregular Galaxy Sagittarius Dwarf Spheroidal Galaxy

Astronomical events	GLEAM-X J162759.5−523504.3 GRB 020813 SN 386

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SWEEPS-04 is a gas giant exoplanet orbiting the Sun-like star SWEEPS J175853.92−291120.6 in the constellation Sagittarius, approximately 27,700 light-years (8,500 parsecs) from Earth.^[1] Discovered in 2006 as part of the Sagittarius Window Eclipsing Extrasolar Planet Search (SWEEPS) program using the Hubble Space Telescope's transit method, it was one of 16 initial candidates identified in the Galactic bulge.^[2] Its planetary nature was confirmed shortly thereafter through radial velocity observations with the European Southern Observatory's Very Large Telescope, detecting the star's gravitational wobble.^[3] The planet has a mass of 3.8 Jupiter masses and a radius of 0.81 Jupiter radii, resulting in a high density for a gas giant, and completes an orbit every 4.2 days at a semi-major axis of 0.055 AU, classifying it as a hot Jupiter.^[4]^[1] The host star, with a mass of 1.24 solar masses and radius of 1.18 solar radii, is an F-type main-sequence star similar to the Sun but slightly hotter and larger.^[1] SWEEPS-04's apparent faintness (stellar magnitude ~18.8) and great distance make it challenging to observe, yet its discovery highlighted the potential for detecting exoplanets in distant stellar populations like the Galactic bulge.^[1] Notable for its extreme distance, SWEEPS-04 ties with SWEEPS-11 as one of the most remote confirmed exoplanets known, providing valuable insights into planetary formation in metal-poor environments far from the Solar System.^[3] The SWEEPS survey's success in identifying short-period transiting planets in crowded fields advanced techniques for exoplanet detection in dense stellar regions.^[2]

Discovery and Observation

SWEEPS Project Overview

The Sagittarius Window Eclipsing Extrasolar Planet Search (SWEEPS) was a Hubble Space Telescope (HST) survey program conducted in 2004 to detect transiting exoplanets in the dense stellar environment of the Galactic bulge. By targeting the Sagittarius window—a low-extinction region allowing deep views into the bulge approximately 8 kpc from the Sun—the project aimed to measure exoplanet occurrence rates around lower-mass stars across a range of metallicities, providing insights into planetary formation and evolution in an ancient stellar population.^[5] Observations spanned seven continuous days from February 22 to 29, 2004, utilizing the Advanced Camera for Surveys (ACS) Wide Field Channel to monitor a 3.4 × 3.4 arcminute field centered at RA 17h 58m 53.4s, Dec −29° 11′ 10″ (J2000). The survey captured approximately 520 images in the F606W (broad V) and F814W (broad I) filters, achieving photometric precision sufficient to detect transits down to ~1% depth for stars brighter than V ≈ 27, while cataloging over 245,000 stars to V ≈ 30. This effort, equivalent to about 100 HST orbits, focused on ~180,000 main-sequence dwarf stars (F, G, K, and M types) to identify short-period transits in a field crowded with blended light from foreground and background sources.^[5] The SWEEPS program identified 16 transiting exoplanet candidates with orbital periods between 0.6 and 4.2 days, including five ultra-short-period planets orbiting in less than one day; of these, five were subsequently confirmed as bona fide exoplanets via ground-based radial velocity follow-up, including SWEEPS-04. These detections demonstrated the feasibility of transit surveys in dense fields and informed models of hot Jupiter frequency in the Galactic bulge, comparable to local occurrence rates.^[5]

Detection and Confirmation

SWEEPS-04 was detected through photometric monitoring of its host star's light curve using the Hubble Space Telescope's Advanced Camera for Surveys (ACS) Wide Field Channel, which revealed periodic dips in brightness indicative of transits.^[6] The observations took place from February 22 to 29, 2004, as part of the SWEEPS program, covering a 3.4 × 3.4 arcmin field in the Galactic bulge.^[6] Light curve analysis employed the box-fitting least-squares algorithm to identify transit signals, with SWEEPS-04 exhibiting a period of 4.200 days and a transit depth of approximately 0.5%, consistent with a large planetary radius relative to the star.^[6] The detection was announced in a paper published by the SWEEPS team, led by Kailash C. Sahu of the Space Telescope Science Institute, confirming SWEEPS-04 as a transiting hot Jupiter candidate among 16 identified in the survey.^[6] The results appeared in Nature on October 5, 2006, marking the first discovery of transiting exoplanets in the Galactic bulge.^[6] Confirmation of SWEEPS-04's planetary nature came from ground-based radial velocity follow-up observations conducted in June 2006 using the UVES spectrograph on ESO's Very Large Telescope (VLT).^[3] These measurements detected a periodic radial velocity variation with a semi-amplitude

K \approx 200

m/s, consistent with the orbital motion induced by a massive planetary companion rather than a stellar or binary system.^[3] The RV data, spanning four nights, provided a best-fit orbital solution matching the photometric period, ruling out false positives such as eclipsing binaries at high confidence.^[3] This combination of transit photometry and spectroscopic confirmation established SWEEPS-04 as a bona fide hot Jupiter with an orbital distance of about 0.055 AU.^[6]

Observational Challenges

Observing SWEEPS-04 presents significant challenges due to its location in the Galactic bulge, approximately 8,500 parsecs (27,710 light-years) away, making it one of the most distant confirmed exoplanets at the time of discovery. This great distance exacerbates the faintness of the host star, which has an apparent magnitude of V=18.8, severely limiting the signal-to-noise ratio in transit observations and necessitating space-based telescopes to achieve sufficient photometric precision.^[1]^[7]^[7] The Sagittarius Window Eclipsing Extrasolar Planet Search (SWEEPS) field is particularly dense with stars, containing thousands of overlapping sources in a small angular area, which complicates the isolation of the host star's light curve from blended neighbors. High stellar crowding in this region, with over 245,000 stars detected to V ~30 in the 202″ × 202″ field of view, requires exceptional angular resolution to resolve individual targets effectively. Additionally, differential extinction and variable reddening across the bulge, characterized by an average E(B-V)=0.64, introduce uncertainties in color-magnitude diagrams and transit depths, further hindering accurate photometry.^[7]^[7]^[7] These obstacles were mitigated through the use of the Hubble Space Telescope's Advanced Camera for Surveys (ACS), which provides high angular resolution of 0.05 arcsec/pixel, enabling the separation of closely spaced stars. Careful point-spread function (PSF) fitting techniques were employed to deblend the light from the host and nearby contaminants, achieving photometric accuracies of ~0.003 mag at V=20. Multi-filter observations in the F606W (V) and F814W (I) bands allowed for corrections to reddening effects, improving the reliability of transit detections in this challenging environment.^[7]^[7]^[7]

Host Star

Stellar Parameters

The host star of SWEEPS-04, designated SWEEPS J175853.92−291120.6, is a main-sequence dwarf located in the Galactic bulge at a distance of approximately 8.5 kpc. Its physical parameters were derived from fitting theoretical isochrones to photometric data obtained during the SWEEPS survey, assuming solar metallicity and an age consistent with the bulge's old stellar population of ~10 Gyr.^[2] Note that for a star of this mass, the main-sequence lifetime is approximately 6 Gyr, indicating the parameters are approximate given the population age. Key stellar parameters are summarized in the following table:

Parameter	Value	Unit
Mass	1.24	M⊙
Radius	1.18	R⊙
Effective temperature	—	K
Surface gravity	—	(cgs)
Metallicity	[Fe/H] ≈ 0.0	dex
Age	~10	Gyr
Luminosity	~1.5	L⊙

These values position the star as slightly more massive and luminous than the Sun, with solar-like metallicity indicative of the typical composition in the bulge environment. The luminosity was computed using the distance modulus and apparent magnitudes in the V and I bands (V = 18.8, I = 17.7). Subsequent analyses of SWEEPS exoplanet hosts, including this star, confirm a preference for metal-rich compositions, with many exhibiting super-solar abundances that enhance planet formation efficiency.^[2]^[8] The age estimate relies on isochrone modeling for the bulge population.^[2]

Spectral Classification

The host star of SWEEPS-04, designated SWEEPS J175853.92−291120.6, has a solar-like spectrum based on observations with the UVES spectrograph on the Very Large Telescope (VLT), showing absorption lines consistent with a main-sequence dwarf similar to solar-type stars.^[6] These observations, conducted in the wavelength ranges 4812–5750 Å and 5887–6759 Å, show strong stellar absorption features that were fitted using a degraded solar template to measure radial velocities.^[6] The star resides at coordinates RA 17h 58m 53.92s, Dec −29° 11′ 20.6″ (J2000) in the constellation Sagittarius, within the Galactic bulge field targeted by the SWEEPS survey.^[6] Its evolutionary stage aligns with isochrone fitting in the survey's color-magnitude diagram, assuming a typical bulge age of ~10 Gyr.^[6] The metallicity of the host star aligns with the average for the Galactic bulge population, [Fe/H] ≈ 0.0 (with a dispersion of ~0.3 dex), indicating formation in the inner Galaxy amid metal-rich conditions prevalent in this region.^[6] Distance estimates place the system at approximately 8,500 pc, confirmed through Galactic models and proper motion data from Hubble Space Telescope observations of the SWEEPS field, corresponding to a distance modulus of (m−M)₀ = 14.3 mag.^[6]

Activity and Variability

High-resolution spectroscopy indicates low stellar activity, with radial velocity measurements showing stability consistent with jitter below 10 m/s, enabling precise orbital determinations for the planet.^[5] This low-activity profile minimizes contamination from stellar phenomena in the transit and radial velocity data.^[5]

Orbital and Physical Characteristics

Orbital Elements

SWEEPS-04 b orbits its host star at a semi-major axis of 0.055 AU, placing it in a close-in configuration typical of hot Jupiters. This distance is derived using Kepler's third law, expressed as

a^3 / P^2 = (M_\star + M_p) / (4\pi^2 / G)

, where

a

is the semi-major axis,

P

is the orbital period,

M_\star

is the stellar mass,

M_p

is the planetary mass, and

G

is the gravitational constant; the approximation holds since

M_\star \gg M_p

. The orbital period is 4.2 days, determined from transit timing analysis of the observed light curve.^[1] The orbit is nearly circular, with eccentricity

e \approx 0

, as constrained by the symmetric transit duration and lack of detectable radial velocity variations indicative of eccentricity. The inclination is approximately

i \approx 90^\circ

, consistent with an edge-on geometry required for transit detection. The transit duration is approximately 3 hours, reflecting the rapid orbital motion at close separation, with an impact parameter

b < 0.5

indicating a central transit across the stellar disk.^[5] Additional orbital elements, such as the longitude of periastron and argument of periastron, remain poorly constrained due to the observation of only a single transit epoch during the SWEEPS survey, limiting the ability to resolve long-term orbital dynamics.

Planetary Mass and Radius

The mass of SWEEPS-04 b is constrained to less than 3.8

M_\mathrm{J}

at the 95% confidence level, derived from radial velocity observations that yielded no detectable semi-amplitude but an upper limit of

K < 0.42

km/s. This limit is calculated using the standard radial velocity formula for a transiting planet:

K = \left( \frac{2\pi G}{P} \right)^{1/3} \frac{M_\mathrm{p} \sin i}{(M_\star)^{2/3} \sqrt{1 - e^2}},

K=(P2πG)1/3(M⋆)2/31−e2

Mpsini, where $P = 4.2$ days is the orbital period, $M_\mathrm{p}$ is the planetary mass, $M_\star = 1.24\, M_\odot$ is the stellar mass, $e \approx 0$ is the eccentricity, and $\sin i \approx 1$ . The observations were conducted with the UVES spectrograph on the Very Large Telescope in 2004.^[5] The radius of SWEEPS-04 b is $0.81 \pm 0.10\, R_\mathrm{J}$ , determined from Hubble Space Telescope photometry in the $V$ and $I$ bands that measured a transit depth of $\delta \approx 0.5\%$ . This value follows from the relation $\delta = (R_\mathrm{p} / R_\star)^2$ , where the host star radius is $R_\star = 1.18\, R_\odot$ , estimated via isochrone fitting to color-magnitude data for the Galactic bulge population.^[5] Given the upper limit on mass and the measured radius, the planetary density has an upper bound of approximately 9.5 g/cm³ (using the nominal 3.8 $M_\mathrm{J}$ value), higher than Jupiter's 1.33 g/cm³ and suggesting a relatively compact gas giant rather than an extremely inflated structure. The equilibrium temperature is approximately 1500 K, calculated assuming zero Bond albedo and efficient redistribution of incident stellar flux across the planetary surface. The host star's metal-poor nature ([Fe/H] ≈ -0.8) suggests lower absolute atmospheric metallicity compared to solar-neighborhood hot Jupiters. As a hot Jupiter, SWEEPS-04 b likely consists of a massive hydrogen-helium envelope surrounding a rocky/icy core of less than 10 $M_\oplus$ , consistent with core-accretion formation models.^[5]^[4]^[2]

Atmospheric Properties

Based on general models for hot Jupiters,¹ SWEEPS-04 b, as a close-in gas giant planet, is expected to possess a hydrogen-dominated atmosphere enriched with trace species such as water vapor, sodium, and potassium, resulting from the intense stellar irradiation that drives photochemical processes and molecular dissociation. Models indicate that high-energy stellar radiation penetrates the upper layers, leading to the presence of atomic sodium and potassium lines, while water vapor persists in deeper, cooler regions despite partial photodissociation. Given the metal-poor host, absolute abundances of rock-forming elements may be lower. The temperature profile of the atmosphere is expected to exhibit a pronounced dayside-nightside dichotomy, with dayside temperatures reaching approximately 1,800 K due to direct stellar heating, while the nightside remains cooler owing to limited horizontal heat transport via winds, which are inefficient in highly irradiated atmospheres. This thermal structure arises from the planet's short orbital period and tidal locking, promoting strong radiative cooling on the nightside and minimal redistribution of heat. A potential thermal inversion in the upper atmosphere may occur, driven by absorption of ultraviolet radiation by titanium oxide (TiO) and vanadium oxide (VO) molecules, which act as strong absorbers and heat the stratosphere above the tropopause. Such inversions are predicted for hot Jupiters with equilibrium temperatures above ~1,500 K, altering emission spectra by elevating stratospheric temperatures. However, lower metallicity may reduce TiO/VO availability. Direct characterization of SWEEPS-04 b's atmosphere via transmission or emission spectroscopy is challenging due to the system's distance of approximately 8,500 parsecs and the faintness of the host star (V ≈ 18.8 mag), rendering observations with current facilities like the Hubble Space Telescope infeasible for high signal-to-noise detections; no such observations have been reported as of 2025. Formation models for close-in giant planets suggest atmospheric metal enrichment relative to the host star's composition, arising from accretion of planetesimals during inward migration through the protoplanetary disk.¹ This enhanced metallicity influences opacity, cloud formation, and radiative transfer, potentially leading to thicker haze layers that mute molecular features in spectra.

Scientific Significance

Role in Exoplanet Demographics

SWEEPS-04, as one of five confirmed hot Jupiters identified in the SWEEPS survey, plays a key role in establishing the demographics of hot Jupiters in the Galactic bulge. These planets indicate an occurrence rate of approximately 0.2% for such close-in giants among bulge stars, a frequency comparable to that observed in the solar neighborhood after accounting for stellar population differences.^[2] This finding highlights the ubiquity of hot Jupiters across diverse Galactic environments, providing a statistical benchmark for population synthesis models. At the time of its discovery in 2006, SWEEPS-04 represented a milestone as one of the most distant confirmed exoplanets known, located approximately 8.5 kpc from Earth in the bulge.^[2] This remoteness extended exoplanet searches to denser, older stellar fields, broadening the known parameter space for habitable zone investigations beyond the local disk. The planet's characteristics bolster theoretical models of planetary migration, where disk interactions drive gas giants to short-period orbits like its 4.2-day period. Observations from the SWEEPS sample indicate that hot Jupiter occurrence rates increase with host star metallicity, consistent with trends in the solar neighborhood.^[2] In contemporary exoplanet catalogs, such as the NASA Exoplanet Archive (accessed 2024), SWEEPS-04 serves as a reference for transiting systems at extragalactic distances, aiding validations of detection pipelines for future bulge surveys.^[1]

Implications for Distant Planet Studies

The discovery of SWEEPS-04 exemplified the Hubble Space Telescope's (HST) capability to perform high-precision transit photometry in the crowded fields of the Galactic bulge, resolving transits around stars separated by as little as 0.085 arcseconds despite differential crowding and extinction challenges. This demonstrated HST's efficacy for bulge surveys, achieving a photometric precision of 0.5–1.0 millimagnitudes over 7 days of monitoring, and laid foundational techniques for deep-field exoplanet detection strategies. Such advancements directly inform the design of James Webb Space Telescope (JWST) programs targeting distant, dust-obscured regions, where infrared capabilities can extend transit surveys to greater volumes and fainter magnitudes.^[10] Radial velocity follow-up observations of the V=18.8 host star using the 8.2-meter Very Large Telescope (VLT) with UVES established an upper limit on SWEEPS-04's planetary mass of less than 3.8 Jupiter masses, with no detectable semi-amplitude above ~420 m/s over four nights, ruling out brown dwarf companions.^[3] This proof-of-concept addressed key challenges in characterizing distant transiting planets, establishing that 8-meter-class telescopes can achieve the necessary signal-to-noise for velocity precision below 100 m/s on faint bulge stars, thereby setting practical limits for confirmation pipelines in future space-based missions. The SWEEPS-04 results guide observational strategies for the Transiting Exoplanet Survey Satellite (TESS) and JWST in the Galactic plane, balancing high crowding that reduces detection efficiency with the potential for elevated planet occurrence rates due to denser stellar populations along sightlines toward the bulge.^[10] These insights emphasize the need for advanced light curve decontamination algorithms to maximize yields in regions where extinction varies rapidly over small angular scales. The distance to the host star is approximately 8.5 kpc.^[1]

Comparison to Other Hot Jupiters

SWEEPS-04 shares notable similarities with other well-known hot Jupiters in its orbital period and estimated mass range. For instance, its orbital period of 4.2 days is comparable to that of HD 209458 b, which orbits with a period of 3.5 days and has a mass of approximately 0.71 M_J. Both planets are classified as hot Jupiters due to their close-in orbits, and HD 209458 b exhibits an inflated radius attributed to tidal heating from ongoing orbital dissipation, a mechanism that may also influence SWEEPS-04 given its similar configuration, though the latter's radius measurement of 0.81 R_J carries substantial uncertainty and its mass is constrained to less than 3.8 M_J, implying a potentially low density.^[5]^[11] In terms of differences, SWEEPS-04 is located at a considerably greater distance of about 8 kpc in the Galactic bulge, in contrast to nearer hot Jupiters such as HAT-P-7 b at roughly 320 pc. The host star of SWEEPS-04 also displays lower metallicity relative to some peers, like WASP-12 with [Fe/H] = +0.3, aligning with the broader and typically sub-solar metallicity distribution observed in bulge stars compared to the metal-rich environments often associated with hot Jupiter hosts in the solar neighborhood.^[5]^[12]^[13] A distinctive feature of SWEEPS-04 is its status as one of the earliest confirmed hot Jupiters in the Galactic bulge, challenging the biases of initial exoplanet surveys that predominantly targeted nearby solar neighborhood stars and thus underrepresented distant populations. This positioning allows for investigations into whether hot Jupiters form and persist similarly around bulge stars, which differ in age, metallicity, and evolutionary history from local counterparts. Regarding physical properties, the inferred upper limit on the density of SWEEPS-04 is consistent with other hot Jupiters, though precise values depend on the unknown true mass below 3.8 M_J.^[5]

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SWEEPS-04

See also

References

External links

SWEEPS-04

Discovery and Observation

SWEEPS Project Overview

Detection and Confirmation

Observational Challenges

Host Star

Stellar Parameters

Spectral Classification

Activity and Variability

Orbital and Physical Characteristics

Orbital Elements

Planetary Mass and Radius

Atmospheric Properties

Scientific Significance

Role in Exoplanet Demographics

Implications for Distant Planet Studies

Comparison to Other Hot Jupiters

Footnotes

References

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