Parsec to Arpent Converter

Convert parsecs to arpents with our free online length converter.

Quick Answer

1 Parsec = 5.277317e+14 arpents

Formula: Parsec × conversion factor = Arpent

Use the calculator below for instant, accurate conversions.

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Last verified: February 2026|Reviewed by: Sam Mathew, Software Engineer

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How to Use the Parsec to Arpent Calculator:

Enter the value you want to convert in the 'From' field (Parsec).
The converted value in Arpent will appear automatically in the 'To' field.
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How to Convert Parsec to Arpent: Step-by-Step Guide

Converting Parsec to Arpent involves multiplying the value by a specific conversion factor, as shown in the formula below.

Formula:

1 Parsec = 5.2773e+14 arpents

Example Calculation:

Convert 10 parsecs: 10 × 5.2773e+14 = 5.2773e+15 arpents

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What is a Parsec and a Arpent?

and Standards

Geometric Definition

The parsec is defined through trigonometric parallax:

1 parsec = the distance at which 1 astronomical unit (AU) subtends an angle of 1 arcsecond (1″)

Mathematically:

1 parsec = 1 AU / tan(1″)
Since 1″ = 1/3600 degree = π/648,000 radians ≈ 4.8481 × 10⁻⁶ radians
For small angles: tan(θ) ≈ θ (in radians)
1 parsec ≈ 1 AU / 4.8481 × 10⁻⁶ ≈ 206,265 AU

Exact IAU Value

The International Astronomical Union (IAU) defines the parsec exactly as:

1 parsec = 648,000/π AU ≈ 206,264.806247 AU

Using the IAU-defined astronomical unit (1 AU = 149,597,870,700 meters exactly as of 2012):

1 parsec = 30,856,775,814,913,673 meters (exactly)

Or approximately:

3.0857 × 10¹⁶ meters
30.857 trillion kilometers
19.174 trillion miles

Relationship to Light-Year

The light-year (distance light travels in one Julian year) relates to the parsec:

1 parsec ≈ 3.26156 light-years

More precisely: 1 pc = 3.261563777 ly (using Julian year of 365.25 days)

Standard Multiples

Kiloparsec (kpc): 1 kpc = 1,000 pc ≈ 3,262 ly

Used for distances within galaxies
Milky Way diameter: ~30 kpc

Megaparsec (Mpc): 1 Mpc = 1,000,000 pc ≈ 3.26 million ly

Used for intergalactic distances
Andromeda Galaxy: ~0.77 Mpc

Gigaparsec (Gpc): 1 Gpc = 1,000,000,000 pc ≈ 3.26 billion ly

Used for cosmological distances
Observable universe radius: ~14 Gpc

The Arpent is a historical French unit used primarily for measuring land area, but also sometimes used as a unit of length. As a unit of length, the arpent typically referred to the side length of a square arpent of land.

Its precise length varied significantly by region and time period in France and its colonies. A commonly cited value, particularly associated with the arpent de Paris, is based on 180 French feet (pieds du Roi), which equates to approximately:

58.47 meters (m)
191.8 feet (ft)

Other variations existed, such as the arpent commun (based on 200 French feet, ~64.97 m) and the arpent d'ordonnance (based on 220 French feet, ~71.47 m).

Note: The Parsec is part of the imperial/US customary system, primarily used in the US, UK, and Canada for everyday measurements. The Arpent belongs to the imperial/US customary system.

History of the Parsec and Arpent

and Evolution

Pre-Parsec Era: The Parallax Quest (1600s-1830s)

The concept of stellar parallax dates to ancient Greek astronomy, but detecting it required centuries of technological advancement.

Galileo Galilei (1610) suggested that if Earth orbits the Sun, nearby stars should show annual parallax shifts against distant background stars. No parallax was detected, leading geocentrists to argue Earth must be stationary.

James Bradley (1728) discovered stellar aberration (apparent star position shifts due to Earth's orbital motion combined with finite light speed), confirming Earth's motion but still failing to detect parallax—stars were simply too distant.

Friedrich Wilhelm Bessel achieved the first successful parallax measurement in 1838 for 61 Cygni, determining a distance of about 10.3 light-years (3.16 parsecs, though the term didn't exist yet). This triumph came using a heliometer—a split-lens telescope enabling precise angular measurements.

Thomas Henderson measured Alpha Centauri's parallax (1832-1833, published 1839), and Friedrich Struve measured Vega's (1837), establishing parallax as the fundamental distance measurement method.

Coining the Term (1913)

Herbert Hall Turner (1861-1930), British astronomer and director of Oxford University Observatory, coined "parsec" in 1913. Before this, astronomers expressed stellar distances awkwardly:

In astronomical units (requiring numbers in the hundreds of thousands)
In light-years (popular but not directly tied to measurement method)
In "parallax seconds" (inverse of parallax angle, but confusing terminology)

Turner recognized that astronomers naturally thought in terms of parallax angles. For a star with parallax angle p (in arcseconds), the distance d is simply:

d (in parsecs) = 1 / p (in arcseconds)

This elegant relationship made the parsec immediately practical. A star with 0.5″ parallax is 2 parsecs away; 0.1″ parallax means 10 parsecs; 0.01″ parallax means 100 parsecs.

IAU Adoption (1922-1938)

The 1922 IAU General Assembly in Rome endorsed the parsec as the standard unit for stellar distances, though adoption wasn't immediate or universal.

The 1938 IAU General Assembly in Stockholm formally standardized the parsec definition based on the astronomical unit and arcsecond, solidifying its status.

By the 1950s, the parsec dominated professional astronomy literature, though popular science continued preferring light-years for general audiences.

Space Age Precision (1960s-Present)

Hipparcos satellite (1989-1993): European Space Agency mission measured parallaxes for 118,000 stars with milliarcsecond precision, extending reliable parsec-based distances to hundreds of parsecs.

Gaia mission (2013-present): ESA's Gaia spacecraft has revolutionized astrometry, measuring parallaxes for 1.8 billion stars with microarcsecond precision. This extends direct parsec measurements to 10,000+ parsecs (10+ kiloparsecs), mapping our galaxy's structure in unprecedented detail.

2012 IAU redefinition: The IAU redefined the astronomical unit as exactly 149,597,870,700 meters (no longer based on Earth's actual orbit, which varies slightly). This made the parsec exactly 648,000/π AU, providing a stable definition independent of Earth's orbital variations.

The term "arpent" likely derives from the Gaulish arepennis, meaning "end of a field," suggesting its origins relate to agricultural land measurement, possibly representing the amount of land that could be plowed in a day. It became a fundamental unit for land surveying in France during the medieval period and remained in use until the adoption of the metric system following the French Revolution.

Regional Variations: Before standardization efforts, the length (and thus area) of the arpent varied considerably across different regions of France. Key variations included:
- Arpent de Paris: Based on a perche (rod) of 18 pieds du Roi (French feet), with the linear arpent (side of the square) being 10 perches, totaling 180 pieds (~58.47 m). The area was 32,400 square pieds.
- Arpent Commun: Based on a perche of 20 pieds, linear arpent of 200 pieds (~64.97 m). Area: 40,000 square pieds.
- Arpent d'Ordonnance (or Arpent des Eaux et Forêts): Based on a perche of 22 pieds, linear arpent of 220 pieds (~71.47 m). Area: 48,400 square pieds. Used primarily for royal forests.
Colonial Usage: The arpent was exported to French colonies, notably:
- New France (Quebec, Canada): The arpent de Paris became the standard for land grants along the St. Lawrence River, shaping the characteristic long, narrow farm plots (rangs).
- Louisiana (USA): The French arpent (usually the arpent de Paris) was used for land measurement before and sometimes after the Louisiana Purchase. Its legacy persists in land titles and some place names.
Metrication: The metric system officially replaced the arpent and other traditional units in France in the late 18th and early 19th centuries, though its use lingered in practice and historical records.

Common Uses and Applications: parsecs vs arpents

Explore the typical applications for both Parsec (imperial/US) and Arpent (imperial/US) to understand their common contexts.

Common Uses for parsecs

Stellar Astronomy and Parallax Measurements

The parsec's primary use is measuring stellar distances via trigonometric parallax:

Parallax formula: d (parsecs) = 1 / p (arcseconds)

Ground-based observatories: Measure parallaxes to ~0.01″ accuracy, reliable to ~100 pc

Hipparcos satellite: Measured parallaxes to ~0.001″ (1 milliarcsecond), reliable to ~1,000 pc (1 kpc)

Gaia spacecraft: Measures parallaxes to ~0.00001″ (10 microarcseconds) for bright stars, reliable to ~10 kpc for many stars

Applications:

Calibrating the cosmic distance ladder (using Cepheid variables, RR Lyrae stars)
Determining absolute magnitudes of stars
Studying stellar populations and galactic structure
Measuring proper motions and space velocities

Galactic Structure and Dynamics

Kiloparsecs (kpc) describe structures within galaxies:

Milky Way structure:

Galactic center (Sagittarius A*): 8.2 kpc from Sun
Galactic disk radius: ~15 kpc
Central bulge: ~1.5 kpc radius
Spiral arms: trace patterns 10-15 kpc in radius
Dark matter halo: extends to ~60 kpc

Rotation curves: Plot orbital velocity vs. distance (in kpc) from galactic center, revealing dark matter

Star formation regions: Giant molecular clouds span 10-100 pc

Globular clusters: Orbit 10-60 kpc from galactic center

Extragalactic Astronomy

Megaparsecs (Mpc) measure distances between galaxies:

Galaxy surveys: Map millions of galaxies to distances of 1,000+ Mpc, revealing large-scale structure (walls, filaments, voids)

Tully-Fisher relation: Links galaxy rotation speed to luminosity, enabling distance estimates in Mpc

Type Ia supernovae: Standard candles for measuring distances to 1,000+ Mpc

Galaxy clusters: Typical separation between major clusters ~10-50 Mpc

Superclusters: Structures spanning 100-200 Mpc (like Laniakea Supercluster containing Milky Way)

Cosmology and Universe Expansion

Megaparsecs and gigaparsecs describe cosmological distances:

Hubble constant (H₀): Measured in km/s per Mpc—describes universe expansion rate

Current value: H₀ ≈ 67-73 (km/s)/Mpc (tension between measurement methods)
Interpretation: Galaxy 1 Mpc away recedes at ~70 km/s; 100 Mpc away recedes at ~7,000 km/s

Hubble's Law: v = H₀ × d (where d is in Mpc, v is recession velocity)

Comoving distance: Cosmological distance accounting for universe expansion, measured in Mpc or Gpc

Redshift surveys: Map galaxy distribution to 1,000+ Mpc (z ~ 0.1-0.3 redshift)

Baryon acoustic oscillations: ~150 Mpc characteristic scale in galaxy distribution, used as "standard ruler"

Astrophysical Research Papers

Parsecs are the default distance unit in professional astronomy journals:

Observational papers: Report star/galaxy distances in pc, kpc, or Mpc

Theoretical models: Express scale lengths in parsecs (e.g., "disk scale length of 3 kpc")

Computer simulations: Use parsec-based units (or comoving kpc/Mpc for cosmological sims)

Standard convention: Professional astronomers think and calculate in parsecs, converting to light-years only for public communication

When to Use arpents

The Arpent (both linear and area) is now largely obsolete for practical measurement but remains historically significant:

Historical Land Surveys: Essential for interpreting old maps, deeds, and land grants in France, Quebec, Louisiana, and other areas formerly under French control (e.g., parts of the US Midwest like Missouri, Illinois, Indiana).
Legal Context: Land descriptions in some regions may still reference original measurements in arpents, requiring conversion for modern understanding.
Historical Research: Understanding the arpent is crucial for historians studying agriculture, settlement patterns, and land tenure systems in French history and its colonial contexts.
Unit of Area: While this page focuses on the length, the arpent is more commonly known and encountered as a unit of area (the square arpent).

Additional Unit Information

About Parsec (pc)

What does "parsec" stand for?

Parsec is a portmanteau of "parallax of one arcsecond."

It represents the distance at which Earth's orbital radius (1 AU) subtends an angle of exactly one arcsecond (1/3600 of a degree). British astronomer Herbert Hall Turner coined the term in 1913 to provide a convenient unit directly tied to the parallax measurement method.

How is a parsec measured?

Parsecs are measured using trigonometric parallax:

Observe a nearby star from Earth when Earth is on one side of its orbit
Observe the same star six months later when Earth is on the opposite side
Measure the apparent shift in the star's position against distant background stars
Half this shift is the parallax angle p (in arcseconds)
Calculate distance: d = 1/p parsecs

Modern method: Space telescopes like Gaia measure parallax angles with microarcsecond precision, enabling distance measurements to thousands of parsecs.

Is a parsec bigger than a light-year?

Yes, one parsec is significantly larger:

1 parsec ≈ 3.26 light-years

More precisely: 1 pc = 3.261563777 ly

Example: Proxima Centauri at 1.3 parsecs equals 4.24 light-years away.

Why the difference matters: Confusing parsecs with light-years introduces 3× error in distances.

Why do astronomers prefer parsecs over light-years?

Astronomers prefer parsecs for several reasons:

1. Direct observational connection: Parallax angle p (arcseconds) directly gives distance d = 1/p (parsecs). No complicated conversion needed.

2. Professional standard: IAU endorsed parsecs in 1922; they're now universal in research papers and textbooks.

3. Convenient multiples: Kiloparsecs (kpc) for galactic distances, megaparsecs (Mpc) for cosmological distances provide natural scales.

4. Hubble constant units: Universe expansion rate naturally expressed in (km/s)/Mpc.

5. Definition stability: Light-year depends on year length definition (tropical, Julian, sidereal); parsec defined purely by geometry.

Light-years remain popular in public communication because "year" is familiar, while "parallax arcsecond" requires technical knowledge.

How many astronomical units are in a parsec?

1 parsec = 206,265 astronomical units (AU) (approximately)

More precisely: 1 pc = 206,264.806247 AU

This number arises from: 1 pc = 1 AU / tan(1″), and since 1″ = π/648,000 radians:

1 pc = 1 AU / (π/648,000) = 648,000/π AU ≈ 206,265 AU

Context: Since 1 AU ≈ 150 million km (Earth-Sun distance), 1 parsec ≈ 31 trillion km.

What is a kiloparsec and megaparsec?

Kiloparsec (kpc): 1 kpc = 1,000 parsecs ≈ 3,262 light-years

Used for: Galactic-scale distances
Examples: Sun to Milky Way center (8 kpc), galaxy diameters (10-50 kpc)

Megaparsec (Mpc): 1 Mpc = 1,000,000 parsecs ≈ 3.26 million light-years

Used for: Intergalactic distances, cosmology
Examples: Andromeda Galaxy (0.77 Mpc), Virgo Cluster (16.5 Mpc), Hubble constant measured in (km/s)/Mpc

Gigaparsec (Gpc): 1 Gpc = 1,000,000,000 parsecs ≈ 3.26 billion light-years

Used for: Large-scale cosmological structures
Example: Observable universe radius (~14 Gpc)

Is the parsec an SI unit?

No, the parsec is not an SI unit. The SI unit of length is the meter (m).

However, the parsec is:

Recognized by the IAU (International Astronomical Union)
Accepted for use with SI in astronomy contexts
Defined exactly in terms of the AU (which is defined exactly in meters)

Why not SI?: The parsec arose naturally from astronomical practice and remains far more practical than expressing stellar distances in meters (which would require numbers like 10¹⁶ to 10²³).

Analogy: Like the electronvolt (eV) in particle physics, the parsec is a specialized unit indispensable to its field despite not being SI.

How far can parallax measure distances?

Ground-based telescopes: ~0.01 arcsecond precision → reliable to ~100 parsecs

Hubble Space Telescope: ~0.001 arcsecond (1 milliarcsecond) → reliable to ~1,000 parsecs (1 kpc)

Hipparcos satellite (1989-1993): ~0.001 arcsecond → 118,000 stars measured to 100-1,000 pc

Gaia spacecraft (2013-present): ~0.00001 arcsecond (10 microarcseconds) for bright stars → reliable to ~10,000 parsecs (10 kpc)

Measured 1.8 billion stars
Revolutionary precision enables mapping entire Milky Way disk

Fundamental limit: Stars beyond 10-20 kpc have unmeasurably small parallaxes with current technology. For greater distances, astronomers use indirect methods (Cepheids, Type Ia supernovae, redshift).

Did Han Solo make the Kessel Run in "less than 12 parsecs"?

Famous Star Wars quote: "She made the Kessel Run in less than twelve parsecs."

The issue: Parsec measures distance, not time. Saying "less than 12 parsecs" for a speed achievement is like saying "I drove to work in less than 5 miles."

Fan explanations (retroactive justifications):

The Kessel Run involves navigating near black holes; a shorter distance means a more dangerous, direct route
Skilled pilots can shave distance by flying closer to gravitational hazards
This reinterprets "12 parsecs" as boasting about route optimization, not speed

Real answer: George Lucas likely confused parsecs with a time unit when writing the script. The line became famous enough that later writers invented explanations making it technically correct.

Takeaway: In real astronomy, parsecs always measure distance, never time.

How do parsecs relate to the Hubble constant?

The Hubble constant (H₀) describes universe expansion and is typically expressed as:

H₀ ≈ 70 (km/s)/Mpc

Interpretation: For every megaparsec of distance, recession velocity increases by ~70 km/s.

Examples using Hubble's Law (v = H₀ × d):

Galaxy 1 Mpc away: recedes at ~70 km/s
Galaxy 10 Mpc away: recedes at ~700 km/s
Galaxy 100 Mpc away: recedes at ~7,000 km/s
Galaxy 1,000 Mpc away: recedes at ~70,000 km/s

Hubble length: c/H₀ ≈ 4,400 Mpc (14.4 billion ly) - characteristic distance scale of observable universe

Why Mpc?: Using megaparsecs keeps Hubble constant values convenient (70 rather than 0.000000000070 if using parsecs, or 2.3 × 10⁻¹⁸ if using SI meters).

What's the farthest distance ever measured in parsecs?

Observable universe radius: ~14,000 Mpc = 14 Gpc (46 billion light-years comoving distance)

Most distant galaxy observed (as of 2023): JADES-GS-z13-0 at redshift z ≈ 13.2

Comoving distance: ~4,200 Mpc (13.7 billion light-years light-travel distance)
Due to universe expansion, it's now ~10,000 Mpc (32 billion light-years) away

Cosmic microwave background: Emitted 380,000 years after Big Bang

Comoving distance to CMB surface: ~14,000 Mpc (46 billion light-years)

Beyond measurement: The observable universe has a finite size (~14 Gpc radius) due to finite age and light speed. Objects beyond this "cosmological horizon" are unobservable because their light hasn't reached us yet.

About Arpent (arpent)

Is the Arpent a unit of length or area?

The Arpent is primarily known as a unit of area, representing a specific parcel of land. However, a linear arpent also exists, defined as the side length of a square whose area is one arpent. This page focuses on the linear arpent. The relationship is direct: Area Arpent = (Linear Arpent)². Because the linear arpent varied, the area also varied.

Where is the Arpent still relevant?

The Arpent is not used for everyday measurements today. Its relevance is almost entirely historical and legal:

Quebec (Canada): Crucial for understanding historical land division and property lines, especially the seigneurial system.
Louisiana (USA): Important for interpreting land titles dating back to the French colonial period.
France: Relevant for historical studies and understanding old documents.
Other former French territories: May appear in historical records (e.g., Mauritius, parts of the US Midwest).

How long is a linear Arpent?

There is no single value, as it varied regionally. Common historical values include:

Arpent de Paris: ~180 French feet ≈ 58.47 meters ≈ 191.8 feet (Most common in Quebec & Louisiana)
Arpent Commun: ~200 French feet ≈ 64.97 meters ≈ 213.2 feet
Arpent d'Ordonnance: ~220 French feet ≈ 71.47 meters ≈ 234.5 feet (Note: The French foot, pied du Roi, was slightly longer than the English foot, approx. 32.48 cm or 12.79 inches).

How does the linear Arpent compare to a Meter or Foot?

The most common linear arpent (~58.47 m) is significantly longer than a meter. (1 Arpent ≈ 58.47 m)
It is also much longer than a foot. (1 Arpent ≈ 191.8 ft)

Is the Arpent an SI unit?

No, the Arpent is not an SI unit. It is a traditional unit from the French system of measurements. The SI base unit for length is the meter (m), and the SI unit for area is the square meter (m²).

Conversion Table: Parsec to Arpent

Parsec (pc)	Arpent (arpent)
0.5	263,865,848,027,227.2
1	527,731,696,054,454.4
1.5	791,597,544,081,681.5
2	1,055,463,392,108,908.8
5	2,638,658,480,272,271.5
10	5,277,316,960,544,543
25	13,193,292,401,361,358
50	26,386,584,802,722,716
100	52,773,169,605,445,430
250	131,932,924,013,613,580
500	263,865,848,027,227,170
1,000	527,731,696,054,454,340

How do I convert Parsec to Arpent?

To convert Parsec to Arpent, enter the value in Parsec in the calculator above. The conversion will happen automatically. Use our free online converter for instant and accurate results. You can also visit our length converter page to convert between other units in this category.

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What is the conversion factor from Parsec to Arpent?

The conversion factor depends on the specific relationship between Parsec and Arpent. You can find the exact conversion formula and factor on this page. Our calculator handles all calculations automatically. See the conversion table above for common values.

Can I convert Arpent back to Parsec?

Yes! You can easily convert Arpent back to Parsec by using the swap button (⇌) in the calculator above, or by visiting our Arpent to Parsec converter page. You can also explore other length conversions on our category page.

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What are common uses for Parsec and Arpent?

Parsec and Arpent are both standard units used in length measurements. They are commonly used in various applications including engineering, construction, cooking, and scientific research. Browse our length converter for more conversion options.

For more length conversion questions, visit our FAQ page or explore our conversion guides.

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