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Messier 74
Messier 74
Messier 74
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Messier 74
The spiral galaxy M74 (in the left bottom corner is the supernova SN 2013ej)
Observation data (J2000 epoch)
ConstellationPisces[1][2]
Right ascension01h 36m 41.7932s[2]
Declination+15° 47′ 01.272″[2]
Redshift0.002192±0.00000300[2]
Heliocentric radial velocity657±1 km/s[2]
Distance30 ± 6 Mly[2]
Apparent magnitude (V)9.4[2]
Characteristics
TypeSA(s)c HII[2]
Number of stars100 billion (1×1011)
Size85,300 ly (26.16 kpc)
(diameter; D25 isophote)[2]
Apparent size (V)10.5′ × 9.5′[2]
Other designations
Phantom Galaxy, IRAS 01340+1532, NGC 628, UGC 1149, MCG +03-05-011, PGC 5974, CGCG 460-014[2]

Messier 74 (also known as NGC 628 and Phantom Galaxy) is a large spiral galaxy in the equatorial constellation Pisces.[a] It is about 32 million light-years away from Earth.[3] The galaxy contains two clearly defined spiral arms and is therefore used as an archetypal example of a grand design spiral galaxy.[4] The galaxy's low surface brightness makes it the most difficult Messier object for amateur astronomers to observe.[5][6] Its relatively large angular (that is, apparent) size and the galaxy's face-on orientation make it an ideal object for professional astronomers who want to study spiral arm structure and spiral density waves. It is estimated that M74 hosts about 100 billion stars.[3]

Observation history

[edit]

M74 was discovered by Pierre Méchain in 1780. He then communicated his discovery to Charles Messier, who listed the galaxy in his catalog.[6]

M74 observed by JWST

In July 2022, it was observed by the James Webb Space Telescope.

Structure

[edit]

M74 has two spiral arms that wind counterclockwise from the galaxy's center. The spiral arms widen as they get farther from M74's center, but one of the arms narrows at the end. The arms deviate slightly from a constant angle.[7]

Supernovae

[edit]

Three supernovae have been observed in M74:

  • SN 2002ap (Type Ic, mag. 14.5) was discovered by Yoji Hirose on 29 January 2002.[8][9] It was one of few Type Ic supernovae (which denotes hypernovae) recorded within 10 Mpc every century.[10][11][12] This explosion has been used to test theories on the origins of others further away[11] and theories on the emission by supernovae of gamma ray bursts.[12] It got as bright as magnitude 12.3, making it the brightest supernova of 2002.[13]
  • SN 2003gd (Type II-P, mag. 13.2) was discovered by Robert Evans on 12 June 2003.[14][15][16] Type II supernovae have known luminosities, so they can be used to accurately measure distances. The distance measured to M74 using SN 2003gd is 9.6 ± 2.8 Mpc, or 31 ± 9 million ly.[17] For comparison, distances measured using the brightest supergiants are 7.7 ± 1.7 Mpc and 9.6 ± 2.2 Mpc.[17] Ben Sugerman found a "light echo" – a later reflection of the explosion – associated with SN 2003gd.[18] This is one of the few supernovae in which such a reflection has been found. This reflection appears to be from dust in a sheet-like cloud that lies in front of the supernova, and it can be used to determine the composition of the interstellar dust.[18][19]
  • SN 2013ej (Type II-P, mag. 13.5) was discovered by the Lick Observatory Supernova Search (LOSS) on 25 July 2013.[20][21] It was bright as 10th magnitude when viewed from the surface of Earth, so it was visible from almost all modern telescopes in a good night sky.[22]

In addition to these supernovae, the astronomical transient AT 2019krl was discovered by Anna Ho on 6 July 2019, and classified as either a type IIn supernova or an LBV in outburst.[23][24] Later analysis argued that it was consistent with known examples of giant LBV eruptions and SN 2008S-like objects.[25]

Galaxy group

[edit]

This is the brightest member of the M74 Group, a group of 5 to 7 galaxies that also includes the peculiar spiral galaxy NGC 660 and a few irregular galaxies.[26][27][28] Different group membership identification methods (ranging from a clear, to likely, to perhaps historic gravitational tie) identify several objects of the group in common,[28] and a few galaxies whose exact status within such groupings is currently uncertain.[28]

M74 as observed with the Spitzer Space Telescope as part of the Spitzer Infrared Nearby Galaxy Survey. The blue colors represent the 3.6 micrometre emission from stars. The green and red colors represent the 5.8 and 8.0 micrometre emission from polycyclic aromatic hydrocarbons and possibly dust.

Suspected black hole

[edit]

In 2005[29][b] the Chandra X-ray Observatory announced its observation of an ultraluminous X-ray source (ULX) in M74, radiating more X-ray power than a neutron star, in periodic intervals of around two hours. It has an estimated mass of 10000 M☉. This is an indicator of an intermediate-mass black hole. This would be a rather uncommon class, in between in size of stellar black holes and the massive black holes theorized to be in the center of many galaxies. Such an object is believed to form from lesser ("stellar") black holes within a star cluster. The source has been given identification number CXOU J013651.1+154547.

Amateur astronomy observation

[edit]

Messier 74 is 1.5° east-northeast of Eta Piscium.[5][6] This galaxy has the second-lowest Earth-surface brightness of any Messier object. (M101 has the lowest.) It requires a good night sky.[6][5] This galaxy may be best viewed under low magnification; when highly magnified, the diffuse emission becomes more extended and appears too faint to be seen by many people.[6] Additionally, M74 may be more easily seen when using averted vision when the eyes are fully dark adapted.[5][6]

See also

[edit]
Wikimedia Commons has media related to Messier 74.

References and footnotes

[edit]
[edit]
Revisions and contributorsEdit on WikipediaRead on Wikipedia

Messier 74

View on Grokipedia
from Grokipedia
Messier 74 (M74), also known as NGC 628 and the Phantom Galaxy, is a grand design spiral galaxy located approximately 32 million light-years away in the constellation Pisces. It is viewed nearly face-on from Earth, showcasing its symmetrical spiral arms adorned with prominent dust lanes, clusters of young blue stars, and glowing pink regions of ionized hydrogen. Discovered in 1780 by French astronomer Pierre Méchain, assistant to Charles Messier, it was added to Messier's catalog as the 74th entry. With an of 10.0 and low , M74 is challenging to observe with small telescopes but reveals intricate details through larger instruments or long-exposure imaging. The spans about 95,000 light-years in diameter, making it slightly smaller than the , and is estimated to contain around 100 billion stars. As the dominant member of the M74 Group—a small cluster of about half a galaxies—it exemplifies a classic Sc-type spiral with well-defined arms and a bright central bulge. M74 has been a prime target for multi-wavelength observations, including those from the in visible and infrared light, which highlight its star-forming regions, and more recent views from the and that probe its core and hot gas. Notably, it has hosted several well-studied supernovae, including the Type II-P event SN 2003gd, whose progenitor was directly identified prior to explosion, and SN 2013ej, providing key insights into core-collapse mechanisms. These events, along with others like SN 2002ap and SN 2019krl, underscore M74's role in advancing research on and galactic dynamics.

General Characteristics

Overview

Messier 74 (M74), also known as NGC 628 and the Phantom Galaxy, is a grand design spiral galaxy classified as morphological type SA(s)c in the constellation Pisces. This face-on orientation provides a clear view of its symmetrical spiral structure, making it an archetypal example of such galaxies. Located approximately 32 million light-years from Earth, the distance was estimated using Cepheid variable measurements as part of broader distance ladder calibrations. The galaxy spans an apparent diameter of about 10.3 arcminutes and has a visual magnitude of 9.4, rendering it observable with small telescopes under good conditions despite its relatively low surface brightness. Its nickname, the Phantom Galaxy, arises from this low surface brightness combined with its nearly perfect face-on view, which causes it to blend subtly into the background sky and challenge visual detection. Messier 74 serves as the brightest member of the M74 Group, a modest assembly of galaxies in the local universe.

Physical Properties

Messier 74 has an estimated total mass of approximately 3×10113 \times 10^{11} solar masses, which encompasses its baryonic components and the surrounding , as derived from rotation curve modeling that accounts for the across the galaxy's extent. This mass places it in a similar scale to other intermediate-mass spiral galaxies, where dominates the overall gravitational binding. The spans a of approximately 95,000 light-years, making it comparable in size to the and allowing for detailed studies of its disk structure. It hosts about 100 billion , contributing to a total of roughly 1.5×10101.5 \times 10^{10} solar masses, with the primarily consisting of low- to intermediate-mass distributed across the disk. Observed nearly face-on with an inclination angle of about 5°, Messier 74 provides an unobstructed view of its internal features, facilitating precise measurements of its kinematics and morphology. Its redshift is measured at 0.00217, corresponding to a recession velocity of 657 km/s relative to the Milky Way, indicating it is part of the local cosmic flow within the Pisces constellation group.

Observational History

Discovery and Cataloging

Messier 74 was first discovered by the French astronomer Pierre Méchain at the end of September 1780, during his systematic search for comets in the constellation Pisces. Méchain, a close collaborator of , identified the object as a faint, hazy patch of light using a small refractor typical of the era, with a focal length of approximately 3.5 feet. Méchain communicated his discovery to Messier, describing it as "quite broad, very dim, and extremely difficult to observe," noting its position near the star . Charles Messier independently verified the discovery on October 18, 1780, and incorporated it as the 74th entry in his renowned catalog of nebulae and star clusters, published in the Connaissance des Temps for 1784. Messier's observation confirmed Méchain's findings, describing the object as a "nebula without star, next to which is a star of eighth magnitude; the nebula is very faint, one can see it only with difficulty." At the time, both astronomers regarded it as a nebula, consistent with the prevailing understanding of such diffuse celestial objects before the nature of galaxies was established. This addition to the Messier catalog highlighted the object's challenging visibility even under optimal conditions, underscoring its low surface brightness. In the , the object received further cataloging attention. observed it during his sweeps in the 1820s and 1830s, initially misclassifying it as a in his General Catalogue of 1864 due to its faint, rounded appearance. This designation was carried over into the (NGC), compiled by J. Louis Emil Dreyer and published in 1888, where it was formally assigned the number NGC 628. Early descriptions from this period consistently emphasized its nebulous, ill-defined structure, with Herschel noting it as "faint, very large, round, gradually pretty suddenly much brighter in the middle." These observations cemented Messier 74's place in astronomical history as one of the faint, enigmatic "nebulae" that would later be recognized as a grand-design viewed nearly face-on.

Professional Observations

The Hubble Space Telescope conducted extensive imaging of Messier 74 beginning around 2002–2003, with observations using the Wide Field Planetary Camera 2 (WFPC2) resolving individual stars within the galaxy's disk and arms, particularly in the context of supernova progenitor studies. These images revealed the face-on view of its grand-design spiral structure, allowing astronomers to study the distribution of young stars and H II regions. Subsequent observations in the 2000s, including Advanced Camera for Surveys (ACS) data from 2003 and 2005, further highlighted supernova remnants and the galaxy's star-forming complexes, providing high-resolution views that confirmed its distance of approximately 32 million light-years through resolved stellar populations. In March 2005, the captured a composite image of Messier 74, detecting an (ULX) in one of its spiral arms, approximately 15 arcseconds from the nucleus. This source, known as M74 X-1, exhibits strong variability with nearly periodic oscillations every two hours, likely due to accretion disk instabilities around a candidate with an estimated mass of 100 to 10,000 solar masses. The detection underscored the presence of extreme X-ray binaries in the galaxy's outer regions, contributing to studies of high-energy phenomena in spirals. The targeted the core of Messier 74 in mid-2022 as part of the Feedback in Emerging extrAgalactic Star clusTers (FEAST) program, using its to penetrate dust-obscured regions. These observations unveiled delicate filaments of gas and dust winding through the spiral arms, along with compact clusters of young, massive stars embedded in molecular clouds, offering insights into the initial stages of and feedback processes. Follow-up observations in October 2024 under the FEAST program revisited the galaxy, capturing the edge regions and highlighting stellar feedback effects. As of November 2025, analyses of JWST data, including a study on the spatial evolution of star clusters, have provided new details on cluster properties and feedback mechanisms in M74. Messier 74 plays a role in calibrations, where its distance has been refined using methods anchored to stars observed in nearby galaxies. Photometric analyses of its brightest stars and companions, calibrated against the , yield a of approximately 30.0 mag (about 32 million light-years), aiding in cross-checks for supernova-based distances and Hubble constant estimates.

Morphological Structure

Spiral Arms and Disk

Messier 74 displays a grand design spiral morphology with two prominent, symmetrical spiral arms that wind counterclockwise from the nucleus, creating a well-defined pattern visible across much of the galaxy's face-on disk. This structure is characteristic of isolated spiral galaxies with minimal perturbations, allowing the arms to maintain their coherence over large radial distances. The arms are traced by concentrations of gas, , and young , which enhance their visibility in and observations. The pitch angle of these spiral arms measures approximately 13 degrees (ranging from 12.8° to 13.9° across wavelengths), reflecting moderately open spirals that facilitate the of density waves. As the arms extend outward, they generally widen, increasing in breadth from the inner regions near the nucleus to the mid-disk, though one arm exhibits narrowing at its outer periphery, introducing a minor deviation from perfect symmetry. This contributes to the galaxy's aesthetic appeal in deep imaging, where the arms appear as sweeping, filamentary features against the fainter interarm regions. The galactic disk extends to approximately 95,000 light-years in diameter, comprising a thin stellar component with embedded lanes of gas and dust that delineate the spiral pattern. The stellar disk is relatively uniform in thickness, with scale heights typical of late-type spirals, while the gas layers provide the raw material for ongoing arm dynamics. This disk structure underscores Messier 74's classification as an Sc-type galaxy, with a dominance of the extended disk over any central concentration. The low of the spiral arms arises from the sparse stellar density within them, resulting in a diffuse glow that has earned the its moniker, the Phantom Galaxy. This faintness is exacerbated by the face-on orientation, spreading the light over a large angular area and requiring for effective . Despite the low brightness, the arms remain discernible in professional surveys due to their contrast with darker dust lanes. Analysis of the rotation curve reveals a flat velocity profile extending out to at least 10 kpc, where orbital speeds plateau around 200 km/s, indicative of significant contribution to maintain dynamical equilibrium beyond the luminous matter distribution. This profile, derived from high-resolution HI mapping, supports models of an extended dark halo enveloping the disk, consistent with observations of similar spiral galaxies.

Nucleus and Star Formation Regions

The nucleus of Messier 74 (NGC 628) features a weak oval distortion in the central region and is classified as an unbarred SAc spiral in the de Vaucouleurs system, featuring a subtle oval distortion rather than a prominent bar. This weak bar, with an ellipticity of approximately 0.17 in the near-infrared K-band at a radius of about 33 arcseconds, drives a circumnuclear ring of , as evidenced by CO absorption features and submillimeter imaging of molecular gas. The central region lacks a strong bulge, contributing to the galaxy's overall grand-design spiral morphology, where the nucleus appears compact and low-luminosity compared to more barred systems. Messier 74 exhibits a global rate of approximately 1.7 solar masses per year, with activity primarily concentrated in HII regions along the spiral arms rather than the nucleus itself. These HII regions, ionized by young massive stars, are prominently observed in Hα emission, highlighting complexes such as the "headlight cloud" in the inner disk, which hosts the galaxy's brightest HII region with a of 6.3 × 10³⁹ erg s⁻¹ and an equivalent of 142 pc. Photometric mapping has identified over 500 such regions, many powered by clusters containing around 100 ionizing O stars, underscoring their role in the galaxy's disk-wide star-forming activity. Recent James Webb Space Telescope (JWST) observations using the Mid-Infrared Instrument (MIRI) at wavelengths of 7.7–21 μm have unveiled dust-obscured starburst zones within these HII complexes, revealing intricate networks of gas and dust filaments that trace embedded massive star birth hidden from optical views. These mid-infrared data, part of the PHANGS-JWST survey, show that polycyclic aromatic hydrocarbons and warm dust are closely associated with the earliest phases of star formation, indicating vigorous, dust-enshrouded activity in regions like the nuclear vicinity and arm segments. The stellar populations in Messier 74's star-forming regions display a young age distribution, dominated by O and B stars with ages of 2–4 million years, which ionize the surrounding gas and drive the observed Hα emission. These massive, short-lived stars, totaling masses of about 3 × 10⁵ M⊙ in prominent complexes, contrast with older populations in the disk, highlighting episodic star formation concentrated in the arms where molecular clouds collapse under self-gravity. Such distributions suggest that the galaxy's evolution is shaped by these young clusters, which contribute disproportionately to the overall luminosity and feedback processes.

Stellar and Dynamic Phenomena

Supernovae

Messier 74 has hosted several notable supernovae since 2000, providing valuable insights into stellar explosions in this nearby spiral galaxy. These events, detected through professional astronomical surveys, highlight the galaxy's active star-forming regions where massive stars undergo core-collapse. One of the earliest was SN 2002ap, a Type Ic supernova discovered on January 29, 2002, by amateur astronomer Yoji Hirose using unfiltered CCD images, appearing at an apparent magnitude of V = 14.5 near its peak brightness. This event reached an absolute peak magnitude of M_B ≈ -16.9, marking it as an energetic hypernova-like explosion with broad spectral lines. Studies of SN 2002ap focused on its potential association with gamma-ray bursts, analyzing its radio and X-ray emissions to explore scenarios of failed GRB progenitors due to baryon-loaded jets. Its similarities to GRB-linked supernovae like SN 1998bw underscored investigations into the diversity of stripped-envelope core-collapse events. SN 2003gd, classified as a Type II-P , was discovered on June 12, 2003, by and peaked at an of approximately 13.2 in July. Archival images from before the explosion identified its as a star with an initial mass of about 8-10 solar masses, marking the first direct of such a for a normal Type II-P . This identification, combined with post-explosion imaging showing the progenitor's disappearance, provided key evidence for the evolutionary pathway of intermediate-mass stars ending in plateau-light-curve . The event's and spectra further allowed distance estimates to Messier 74 via the expanding method, yielding approximately 9.3 Mpc. In 2013, SN 2013ej emerged as another Type II-P (or transitional II-L) , discovered on July 25 by the Lick Observatory Supernova Search at an initial magnitude near 13.5, with its peak reaching M_V ≈ -17.8. Extensive multicolor photometry from 8 to 185 days post-explosion revealed a luminous and rapidly declining , atypical for standard II-P events, prompting detailed studies of its early evolution and potential interaction with circumstellar material. Spectroscopic monitoring over 450 days highlighted deviations in its plateau phase, contributing to models of asphericity and dust formation in Type II . More recently, the transient AT 2019krl was detected on July 6, 2019, by Anna Ho using the , reaching an of around 16 and debated as either a Type IIn or a outburst. observations captured a peak of M_{4.5μm} ≈ -18.4, while optical data suggested similarities to imposters like SN 2008S-like events or massive-star mergers. Pre-explosion Hubble images identified a progenitor, fueling ongoing classification debates and studies of eruptive mass loss in massive stars. These at least four confirmed or candidate events since 2000 underscore Messier 74's vigorous stellar evolution, with a supernova rate consistent with its star formation activity in the spiral arms.

Suspected Central Black Hole

In 2005, the Chandra X-ray Observatory identified an ultraluminous X-ray source (ULX) designated CXOU J013651.1+154547, also known as M74 X-1, within Messier 74, approximately 2 kpc from the galaxy's nucleus. This source exhibits a peak luminosity of approximately 104010^{40} erg s−1^{-1} in the 0.3–10 keV band, exceeding the Eddington limit for stellar-mass black holes by orders of magnitude and prompting suggestions of an accreting intermediate-mass black hole (IMBH) with a mass in the range of 10,000 to 100,000 solar masses. Spectral analysis of the Chandra data reveals thermal disk emission characterized by a blackbody temperature of about 0.3 keV, which is inconsistent with standard models for accreting stellar-mass black holes or neutron stars, as such objects would require extreme super-Eddington accretion rates to achieve the observed luminosity. The source shows extreme variability, with flux changes by more than an order of magnitude over timescales of thousands of seconds, including flares and quasi-periodic oscillations on roughly two-hour intervals, consistent with instabilities in the accretion disk around an IMBH. Follow-up observations with in 2009 and subsequent archival data through 2021 confirmed the source's long-term variability and spectral evolution between flaring and non-flaring states, with spectra best fitted by models combining a thermal and Comptonization components or dual-temperature disk blackbody emission. However, as of 2025, no definitive confirmation of the 's mass has been achieved, and alternative interpretations include beamed emission from a stellar-mass or a highly super-Eddington accreting .

Galactic Environment

Messier 74 Group

The Messier 74 Group is a small, loosely bound aggregation of galaxies located in the constellation Pisces, with Messier 74 (NGC 628) as its brightest and central member. This group, also known as the NGC 628 Group, consists of approximately five to seven galaxies, predominantly spirals and irregulars, spanning a physical extent of roughly 1 Mpc. Confirmed members include the peculiar edge-on NGC 660, classified as SB(s)a pec, along with several dwarf irregulars such as UGC 1176 (Im), UGC 1195 (Sc), and UGC 1200 (IBm). These galaxies share consistent distances of about 30–40 million light years and recession velocities in the range of 650–800 km/s, supporting their gravitational binding as a coherent structure. The group is classified as poor or irregular, characterized by its limited membership and absence of a dominant , distinguishing it from richer clusters. The low velocity dispersion of approximately 150 km/s among members further indicates a dynamically relaxed, unbound-like system rather than a tightly interacting cluster.

Nearby Galaxies and Interactions

Messier 74, as the dominant member of the M74 Group, experiences gravitational influences primarily from its sparse companions, including the peculiar spiral NGC 660, though no evidence supports ongoing major mergers. Observations indicate possible minor tidal interactions with companions, manifested in distortions to the southern spiral (S1) and a bent magnetic (I2) in the outer disk, where high magnetic field ordering (>60%) and a sharp neutral (HI) emission gradient suggest shearing from external forces. Similarly, a past with NGC 660 approximately 2 billion years ago may have contributed to the galaxy's multi-armed spiral structure, as inferred from kinematic modeling of density waves. These minor encounters lack signs of recent disruption within the last 1 Gyr, preserving the galaxy's grand-design morphology while potentially triggering localized bursts through enhanced gas compression. HI mapping reveals an extended gaseous envelope around Messier 74, extending well beyond its optical disk and Holmberg radius, with deviations in indicating an unsettled structure. This envelope, while prominent, does not appear attributable to recent tidal interactions but may reflect primordial accretion or subtle . However, tidal stresses from nearby companions could warp portions of this HI layer, contributing to elevated velocity dispersions in molecular clouds comparable to observed values (~5-10 km/s), thereby influencing gas dynamics without major morphological changes. Such effects align with the M74 Group's loose configuration, where limited close passages foster isolated evolution. The M74 Group's dynamical youth, characterized by low velocity dispersion and sparse membership, underscores Messier 74's relative isolation within the broader local supercluster, minimizing opportunities for significant disruptions as of 2025 observations. No simulations confirm recent close passages within ~100 million years, but the absence of tidal tails or bridges supports a history of gentle perturbations rather than violent encounters. This environment allows Messier 74's disk to maintain stability, with external playing a secondary role in its ongoing evolution.

Amateur Observation

Visibility and Location

Messier 74 possesses equatorial coordinates of 01h 36m 42s and +15° 47′ 01″ (J2000 ). It lies in the constellation Pisces, positioned 1.5° east-northeast of the star η Piscium. In the , Messier 74 offers optimal visibility during the autumn season from to , when it culminates at an altitude of approximately 65° as observed from 40°N latitude. Its apparent size of roughly 10 by 9 arcminutes and low of μ_B = 23.4 mag/arcsec² render it challenging to observe without dark, clear skies. In the , Messier 74 is best observed during the spring months from to .

Viewing Techniques

Observing Messier 74 presents unique challenges for astronomers due to its low and large apparent size, requiring specific equipment and strategies for success. A with a minimum of 4 to 6 inches enables visibility of the galaxy's core as a faint, ghostly patch under very , while apertures of 8 inches or larger are necessary to discern the spiral arms and additional details. Optimal conditions involve Bortle class 1-3 skies to minimize , which can easily obscure the galaxy's diffuse glow. To enhance contrast against the , —shifting the gaze slightly away from the object to utilize the eye's more sensitive —is essential for detecting the faint structure. filters, particularly those targeting H-alpha emission from star-forming regions, can further improve visibility of these subtle features by blocking unwanted light. Magnifications between 50x and 100x strike the best balance, providing a wide enough to frame the while resolving central details without over-magnifying the low-contrast disk. Light pollution poses a significant obstacle, often rendering Messier 74 invisible from urban or suburban sites, so observers should prioritize remote locations. For , equatorial tracking mounts are recommended to facilitate long exposures, compensating for the galaxy's faintness and allowing stacked images to reveal its spiral structure. In the , amateur astrophotographers have produced notable images of Messier 74 using DSLR cameras and CCD sensors, often from dark-sky sites, which have heightened public appreciation of this elusive .

References

  1. https://science.nasa.gov/mission/hubble/science/explore-the-night-sky/hubble-messier-catalog/messier-74/
  2. https://science.nasa.gov/asset/hubble/spiral-galaxy-m74/
  3. https://science.nasa.gov/photojournal/a-spiral-galaxy-is-visited-by-a-trojan-war-hero/
  4. https://arxiv.org/abs/astro-ph/0307226
  5. https://arxiv.org/abs/1611.07930
  6. http://www.messier.seds.org/m/m074.html
  7. https://www.messier-objects.com/messier-74-phantom-galaxy/
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