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Messier 43
Messier 43
Messier 43
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Messier 43
Emission nebula
H II region
Emission nebula Messier 43 to the northeast of the well-known M42 Orion Nebula
Observation data: J2000 epoch
Right ascension05h 35m 31.8s[1]
Declination−05° 17′ 57″[1]
Distance1,300 ± 160 ly (400 ± 50 pc) ly
Apparent magnitude (V)9.0[2]
Apparent dimensions (V)20′ × 15′[3]
ConstellationOrion
Notable featuresTrapezium cluster
DesignationsDe Mairan's Nebula, M43, NGC 1982[4]
See also: Lists of nebulae

Messier 43 or M43, also known as De Mairan's Nebula and NGC 1982, is a star-forming nebula with a prominent H II region in the equatorial constellation of Orion. It was discovered by the French scientist Jean-Jacques d'Ortous de Mairan some time before 1731,[3] then catalogued by Charles Messier in 1769.[a] It is physically part of the Orion Nebula (Messier 42), separate from that main nebula by a dense lane of dust known as the northeast dark lane.[5] It is part of the much larger Orion molecular cloud complex.

The main ionizing star in this nebula is the quadruple star system NU Orionis (HD 37061), the focus of the H II region, 1,360 ± 30 ly (417.0 ± 9.2 pc) away.[6]

The H II region is a roundish volume of ionized hydrogen. It has a diameter of about 4.5′, at its distance meaning it measures 2.1 ly (0.65 pc). The net (meaning omitting the star) hydrogen alpha luminosity of this region is (3.0±1.1)×1035 erg s−1; equivalent to 78 L☉. There is a dark lane crossing the whole west-centre strip from north to south, known as the M43 dark lane, which forming a swirling belt extension to the south links to Orion's northeast dark lane. All of these resemble a mixture of smoke rising from a chimney and in watercolour broad and fine dark brushstrokes, at many wavelengths.

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Messier 43

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Messier 43, also known as De Mairan's Nebula, is a compact and active star-forming region in the constellation Orion, situated approximately 1,400 light-years from . It spans an angular size of about 20 by 15 arcminutes and has an of 9.0, making it visible to amateur astronomers using small telescopes under dark skies. Adjacent to the larger (Messier 42), from which it is separated by a prominent dark lane of interstellar dust, Messier 43 is illuminated and sculpted by the ultraviolet radiation from its central massive B0.5 V star, the quadruple system NU Orionis. First recognized as a distinct nebula by French astronomer Jean-Jacques d'Ortous de Mairan in 1731, who described it as a luminous patch surrounding a star, Messier 43 was later cataloged separately by in 1769 during his survey of deep-sky objects to aid comet hunters. As part of the expansive , it represents a blister-type where ionized hydrogen gas glows due to excitation by young, hot stars, fostering ongoing amid dense clouds of gas and dust. The nebula's structure features warped filaments of gas and dust, with intricate details revealed through observations in visible and wavelengths by telescopes like the , highlighting embedded protostars and outflows from nascent stellar systems. Its proximity and brightness make Messier 43 a key target for studying early and the dynamics of molecular clouds, contributing to our understanding of star birth in the . Best observed during winter months in the , it lies near the prominent "sword" of Orion, enhancing its accessibility for both professional and amateur astronomers.

History

Discovery

Messier 43 was first observed and described by the French astronomer and physicist Jean-Jacques d'Ortous de Mairan before 1731. De Mairan, who served as the perpetual secretary of the Académie Royale des Sciences from 1740 until his death in 1771, documented the object in his 1733 publication Traité physique et historique de l'Aurore Boréale, where he referred to it as a brilliance surrounding the star ν Orionis (HD 37061), "very similar to the atmosphere of our Sun, if it were dense enough & extensive enough to be visible in Telescopes at a similar distance." Using a simple refractor typical of early 18th-century instruments, de Mairan noted the feature as a distinct patch of light adjacent to the (M42). This observation highlighted M43's separation from the brighter by a dark lane of dust, marking it as an independent nebulous region amid the limited deep-sky surveys of the era. De Mairan's account lacked precise coordinates, relying instead on qualitative proximity to the trapezium stars in Orion, yet it stands as the earliest recorded recognition of M43 as a separate entity. In the context of 18th-century astronomy, when telescopic observations were advancing through figures like and , de Mairan's work exemplified the growing interest in resolving faint celestial phenomena beyond naked-eye visibility. This initial identification laid the groundwork for its later formal inclusion in Charles Messier's catalog in 1769.

Cataloging

Charles Messier independently rediscovered and cataloged Messier 43 on March 4, 1769, as the 43rd entry in his catalog of nebulae and star clusters compiled during his comet-hunting efforts, describing it as a "little mass of about 3′ extent, of nebulosity, in which are 3 or 4 small stars." This entry followed his earlier observation of the nearby (M42) on the same date, though he assigned separate designations to distinguish the features separated by a dark lane. Prior to Messier's cataloging, the feature had been noted by the French astronomer Jean-Jacques d'Ortous de Mairan before 1731 and published qualitatively in 1733 without coordinates. In 1888, John Louis Emil Dreyer included the object as NGC 1982 in the of Nebulae and Clusters of Stars, describing it as "vB, vL, R with tail np, mbM" (very bright, very large, round with a tail to the north preceding, much brighter in the middle), based on observations by and others. Messier 43 became known alternatively as De Mairan's Nebula in honor of its initial observer, a name popularized in 19th-century astronomical literature. During that century, surveys such as those by the Herschels increasingly recognized it as an integral component of the broader Orion Nebula complex, mapping its position relative to surrounding nebulosity and dark lanes. The object's classification evolved from a generic "nebula" in 18th- and 19th-century descriptions to an identified gaseous emission nebula through spectroscopic analysis, with William Huggins' 1864 observations revealing bright emission lines indicative of incandescent gas. By the early 20th century, advancements in spectroscopy confirmed its nature as an H II region of ionized hydrogen, excited by embedded hot stars, as detailed in studies by Vesto Slipher and others examining nebular spectra.

Location and Visibility

Coordinates

Messier 43 is situated in the constellation Orion, immediately adjacent to the prominent Belt asterism formed by , , and , positioning it within the sword region pointing southward from the belt. The nebula's equatorial coordinates in the J2000 epoch are 05ʰ 35ᵐ 31ˢ and −05° 16′ 12″. Its corresponding galactic coordinates are longitude 208.9° and latitude −19.3°. Messier 43 lies approximately 7 arcminutes north of the Trapezium asterism (θ¹ Orionis), the central star cluster of the adjacent (M42), from which it is physically connected but visually separated by a prominent dark dust lane.

Observing Conditions

Messier 43 has an of 9.0, rendering it invisible to the but detectable as a faint glow adjacent to the brighter (M42) using or telescopes with at least a 50 mm under dark skies. Its angular size spans 20′ × 15′, presenting as a distinctive comma-shaped patch of nebulosity that surrounds the star NU Orionis and is separated from M42 by a prominent dark lane. Optimal visibility occurs during the winter months of December to February from locations above 20°N , when the object culminates near midnight in , positioning it high overhead for extended observation. Southern Hemisphere observers can view it with a clear southern horizon, though it appears lower in the sky and requires sites with minimal atmospheric interference. Positioned just south of , it benefits from the constellation's prominence during this period. Observing challenges include severe obscuration by , which diminishes its faint emission, necessitating dark-sky sites away from urban areas. The overwhelming brightness of nearby M42 often overwhelms M43's subtler features, making essential and OIII filters useful to isolate its emission lines and enhance contrast against the background.

Physical Characteristics

Distance and Size

Messier 43 lies within the at a of 410 ± 20 parsecs (approximately 1,340 ± 65 light-years) from , as measured using data from the Data Release 3 for its central ionizing HD 37061. This trigonometric is corroborated by spectroscopic methods, which yield 430 ± 50 parsecs based on extinction-corrected flux and visual magnitude analysis of the same system. Prior determinations, relying on Very Long Baseline Array observations of associated stellar sources, adopted a similar value of 400 ± 50 parsecs. The spans an of about 20 arcminutes, corresponding to a physical extent of roughly 2.4 parsecs (approximately 7.8 light-years) across at the distance, encompassing a volume of ionized gas. Its bright core, a compact , is more limited, measuring around 4.5 arcminutes in diameter or 0.65 parsecs (about 2.1 light-years), as delineated by Hα and Hβ emission imaging. The structure exhibits an expansion rate with an outflow of approximately 6 km/s, derived from velocity-resolved [C II] emission observations revealing a bubble-like driven by the central . Age estimates from dynamical modeling of the stellar system place the at around 2.5 ± 0.5 million years, aligning with the evolutionary timeline of the surrounding Orion region.

Morphology

Messier 43 exhibits a distinctive comma-shaped morphology, characterized by a bright core that fans out into elongated tendrils of ionized gas, spanning an angular extent of approximately 20′ × 15′. This fan-like structure is sculpted by the intense radiation from its central ionizing star, creating a dynamic landscape of emission features within the broader . A prominent dark lane of interstellar dust visually separates Messier 43 from the adjacent (M42), enhancing its isolated appearance while highlighting the turbulent interface between the ionized region and surrounding molecular material. The nebula's internal structure reveals intricate filaments and knots of gas, particularly evident around embedded young stars still shrouded in dust cocoons, as captured in high-resolution imagery combining visible and near-infrared wavelengths. These filaments trace the pathways of stellar winds interacting with the ambient medium, contributing to the nebula's irregular, asymmetrical form. As a classic , Messier 43 is primarily composed of ionized and , with the reddish hue in visible light arising from emission lines, while dust lanes preferentially absorb shorter blue wavelengths, reddening the overall appearance. Substructures include a bright rim along the edge facing the central star, where photoevaporation erodes the surrounding , producing enhanced and glow at the boundary. This compact, roughly spherical envelope of plasma, with a diameter of about 4.5 arcminutes in its core, underscores the region's role as a stellar nursery shaped by radiative feedback.

Stellar Content and Ionization

Ionizing Star

The primary ionizing star of Messier 43 is NU Orionis, also designated HD 37061, a massive early-type star of spectral type B0.5 V that emits intense radiation responsible for the nebula's illumination. This star exhibits high indicative of its youth and rapid , dominating the energy input to the surrounding gas cloud. Key physical properties of NU Orionis include a of approximately 19 M⊙, a radius of about 8.2 R⊙, a surface of roughly 31,500 , and a bolometric of around 92,000 L⊙. It forms part of a quadruple system, consisting of a close spectroscopic binary (Aa-Ab, SB1, mass ratio of the secondary to primary around 0.19), a close visual companion C separated by approximately 8.6 mas, and an additional visual companion B separated by approximately 470 mas with a flux ratio of 0.03. The ionization mechanism relies on ultraviolet photons from NU Orionis, which have energies above 13.6 eV and strip electrons from hydrogen atoms in the surrounding neutral gas, producing the characteristic H II region of ionized plasma. The rate of ionizing photons (N_γ) emitted by the star is approximately 10^{47.2} s^{-1}, enabling the creation and maintenance of the nebula's structure. This process can be modeled using the Strömgren sphere approximation for a spherical H II region in equilibrium, where the radius R_s is given by Rs=(3Nγ4παBn2)1/3,R_s = \left( \frac{3 N_\gamma}{4 \pi \alpha_B n^2} \right)^{1/3}, with α_B as the case-B hydrogen recombination coefficient (typically ~2.6 × 10^{-13} cm³ s^{-1} at 10^4 K) and n as the ambient hydrogen density (~500 cm^{-3}). Substituting these values yields R_s ≈ 0.3 pc, which closely approximates the observed half-size of Messier 43 (~0.32 pc radius, corresponding to an angular diameter of ~4.5 arcmin at a distance of 410 pc), confirming the star's role in bounding the ionized volume. NU Orionis displays irregular photometric variability, with visual magnitude fluctuating between 6.80 and 6.93, likely driven by instabilities in its stellar winds and potential minor eruptive episodes common in hot massive stars.

Embedded Stars

Messier 43 hosts a population of embedded stars primarily associated with a compact mini-cluster centered on the ionizing star NU Orionis, forming part of the broader in the complex. This mini-cluster includes a small population of young stars, mostly low-mass pre-main-sequence objects, with the dominant illumination from NU Orionis. Approximately 50 young stellar objects (YSOs) have been detected in the core via observations. These stars, with ages less than 1 Myr, are embedded in dense gas and dust, contributing to the region's active environment. Notable among the embedded population are several Herbig-Haro objects, which arise from bipolar outflows of material ejected by young stars interacting with the surrounding . These outflows trace the dynamical processes of early . Pre-main-sequence stars in the cluster exhibit characteristics typical of very young systems, including protoplanetary disks and accretion activity, further evidenced by infrared excesses. Recent JWST NIR and MIR imaging has identified proplyds and jets in M43, such as a giant proplyd (332-1605) and a new candidate with a prominent jet, highlighting active outflows. The mini-cluster dynamics suggest hierarchical formation, where substructures coalesce within the larger Orion Nebula Cluster, with a total estimated mass of 100-200 M⊙M_\odot. Infrared observations from Spitzer and more recent JWST surveys have been crucial for detection, penetrating the obscuring dust to reveal the YSOs, many classified as Class I and II protostars with dusty envelopes. These detections highlight the embedded nature of the population, with Spitzer identifying mid-infrared variability in about 50% of the YSOs, indicating ongoing disk evolution.

Scientific Significance

Star Formation

Messier 43 represents an active site of star formation within the , driven by in dense molecular cores that leads to the formation of protostars. High-resolution submillimeter observations have identified several young stellar objects (YSOs) in M43 surrounded by massive protoplanetary disks, with masses ranging from 0.018 to 0.066 M_⊙ and radii up to approximately 300 AU, providing evidence of the disk accretion phase during early . These disks, observed around low-mass protostars such as those with spectral types K5 and M2.5, indicate ongoing mass accumulation and potential planet formation, while associated outflows and jets—detected in the broader Orion region through and radio imaging—reveal the ejection of material from these YSOs as they clear their envelopes. Molecular line surveys using CO (2-1) transitions have mapped the in the M42/M43 region, revealing two distinct velocity components at approximately 8 km s^{-1} and 13 km s^{-1} with complementary spatial distributions, consistent with a cloud-cloud collision that compressed gas and initiated collapse about 0.1 Myr ago. This triggering mechanism is associated with the formation of the central B-type star in M43. The rate in the region is estimated at ~10^{-4} M_⊙ yr^{-1}. and stellar winds from the massive ionizing star NU Ori erode the surrounding molecular clouds in M43, sculpting the nebula and potentially compressing nearby dense clumps to trigger additional low-mass in evaporating gaseous globules (EGGs) or analogous photoevaporating structures. Multi-wavelength imaging from facilities like Spitzer and Herschel traces the evolutionary progression in M43, from deeply embedded Class 0/I protostars with thick infalling envelopes and high bolometric temperatures around 30-50 K, to more evolved Class II stars exhibiting cleared inner disks and increased near-infrared emission. These observations highlight M43's role in producing a diverse amid feedback-driven disruption, including ~4 proplyds identified in recent JWST imaging.

Research Highlights

Early spectroscopic studies of Messier 43 in the 1910s, led by Vesto M. Slipher at , identified prominent emission lines such as Hα and [O III] in the nebula's spectrum, confirming its gaseous nature and excitation by nearby massive stars. These observations established the foundational understanding of M43 as an , with bright-line spectra indicating processes. By the 1970s, detailed analyses refined measurements of physical conditions, including electron densities on the order of 10^3–10^4 cm⁻³ derived from forbidden line ratios like [S II] λ6717/λ6731. Advancements in the 1990s and 2010s came from imaging, which resolved intricate filaments of gas and dust sculpted by stellar radiation and winds in M43. These high-resolution views, using filters like F555W and F814W, highlighted the nebula's structure around the central B0.5 V star NU Orionis, revealing proplyds and ionization fronts at scales of arcseconds. More recently, observations from 2022, part of the PDRs4All program targeting the broader Orion complex, have imaged proplyds and jets in M43, including a prominent jet in candidate proplyd 269–1713. Key quantitative insights include the nebula's net Hα luminosity of (3.0 ± 1.1) × 10^{35} erg s^{-1}, corrected for and diffuse emission, which quantifies the ionization rate and energy budget. Photoionization models balance recombination rates with incident ionizing photons, following the equilibrium equation nenpαB=∫ν0∞Nγ(ν)V dνn_e n_p \alpha_B = \int_{ \nu_0 }^\infty \frac{N_\gamma(\nu)}{V} \, d\nu, where nen_e and npn_p are and proton densities, αB\alpha_B is the case-B recombination coefficient, Nγ(ν)N_\gamma(\nu) is the flux, and VV is the volume; such models reproduce observed line ratios and electron densities around 500–600 cm^{-3} in M43's core. Recent gaps in distance estimates have been addressed by Data Release 3 (2022), yielding a refined value of approximately 393 ± 13 pc for the complex, including M43, improving geometric constraints on its size and dynamics. Ongoing Atacama Large Millimeter/submillimeter Array (ALMA) surveys continue to probe the molecular content, mapping CO and other tracers to reveal embedded gas reservoirs and their role in within M43.

References

  1. https://science.nasa.gov/mission/hubble/science/explore-the-night-sky/hubble-messier-catalog/messier-43/
  2. https://www.stsci.edu/~harrisj/Documents/aj_140_4_985.pdf
  3. https://apod.nasa.gov/apod/ap150710.html
  4. http://www.messier.seds.org/xtra/history/mairan_o.html
  5. http://www.messier.seds.org/Bios/demairan.html
  6. https://science.[nasa](/page/NASA).gov/mission/hubble/science/explore-the-night-sky/hubble-messier-catalog/messier-43/
  7. http://www.messier.seds.org/xtra/history/m-cat.html
  8. http://www.messier.seds.org/m/m043.html
  9. https://archive.org/details/newgeneralcatalo00dreyrich
  10. https://simbad.cds.unistra.fr/simbad/sim-basic?Ident=M+43
  11. https://www.go-astronomy.com/messier.php?Messier=M43
  12. https://astropixels.com/diffusenebulae/M43-01.html
  13. https://www.messier-objects.com/messier-43-de-mairans-nebula/
  14. https://www.aanda.org/articles/aa/full_html/2024/11/aa51878-24/aa51878-24.html
  15. https://www.aanda.org/articles/aa/full_html/2011/06/aa16608-11/aa16608-11.html
  16. https://arxiv.org/abs/2005.03917
  17. https://www.ing.iac.es/PR/clippings/astronow.pdf
  18. https://esahubble.org/images/potw1109a/
  19. https://arxiv.org/pdf/2410.23229
  20. https://arxiv.org/abs/1209.3826
  21. https://www.aanda.org/articles/aa/full_html/2024/05/aa46747-23/aa46747-23.html
  22. https://iopscience.iop.org/article/10.1088/0004-6256/150/4/108
  23. https://arxiv.org/pdf/0906.1400
  24. https://iopscience.iop.org/article/10.3847/1538-4357/aac217
  25. https://ui.adsabs.harvard.edu/abs/1997AJ....113.1733H/abstract
  26. https://lweb.cfa.harvard.edu/irac/publications/2005other/orion.pdf
  27. https://www.researchgate.net/publication/234453032_On_the_Spectra_of_the_Orion_Nebulosities
  28. https://ui.adsabs.harvard.edu/abs/2025ARep...69..157V/abstract
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